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Coordinates: Sky map 10h 56m 28.99s, +07° 00′ 52″
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{{short description|Red dwarf in the constellation Leo}}
{{short description|Red dwarf in the constellation Leo}}
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{{about|the star|the fictional battle|The Best of Both Worlds (Star Trek: The Next Generation){{!}}The Best of Both Worlds (''Star Trek: The Next Generation'')|''The Outer Limits'' episode|Wolf 359 (The Outer Limits){{!}}Wolf 359 (''The Outer Limits'')|the podcast|Wolf 359 (podcast){{!}}''Wolf 359'' (podcast)}}

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{{about|the star|the fictional Star Trek battle|Battle of Wolf 359|the The Outer Limits episode|Wolf 359 (The Outer Limits)|the podcast|Wolf 359 (podcast)}}
{{Sky|10|56|28.99|+|07|00|52|7.78}}
{{Sky|10|56|28.99|+|07|00|52|7.78}}
{{Starbox begin
{{Starbox begin
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| epoch=J2000
| epoch=J2000
| constell=[[Leo (constellation)|Leo]]
| constell=[[Leo (constellation)|Leo]]
| ra={{RA|10|56|28.921}}<ref name=edr3/>
| ra={{RA|10|56|28.92087}}<ref name=dr3/>
| dec={{DEC|+07|00|53.00}}<ref name=edr3/>
| dec={{DEC|+07|00|53.0033}}<ref name=dr3/>
| appmag_v=13.54<ref name="SIMBAD" />
| appmag_v=13.507<ref name=aj137_5/>
}}
}}
{{Starbox character
{{Starbox character
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| u-b=+1.165<ref name=aj137_5/>
| u-b=+1.165<ref name=aj137_5/>
| variable=[[Flare star|UV Ceti]]<ref name=ass95_2/>
| variable=[[Flare star|UV Ceti]]<ref name=ass95_2/>
| appmag_1_passband=J<!-- Passband for second apparent magnitude (e.g., H, J, K, etc.) -->
| appmag_1_passband=J
| appmag_1=7.1<ref name="SIMBAD"/>
| appmag_1=7.1<ref name=2mass/>
| appmag_2_passband=K
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| appmag_2=6.1<ref name=2mass/>
}}
}}
{{Starbox astrometry
{{Starbox astrometry
| radial_v=+19 ± 1<ref name=apj583/>
| radial_v={{val|+19|1}}<ref name=apj583/>
| prop_mo_ra=–3,866<ref name=edr3/>
| prop_mo_ra={{val|-3866.338|fmt=commas}}
| prop_mo_dec=–2,699<ref name=edr3/>
| prop_mo_dec={{val|-2699.215|fmt=commas}}
| pm_footnote=<ref name=dr3/>
| parallax=415.1794
| parallax=415.1794
| p_error=0.0684
| p_error=0.0684
| parallax_footnote=<ref name=edr3>{{cite Gaia EDR3|3864972938605115520}}</ref>
| parallax_footnote=<ref name=dr3/>
| absmag_v=16.65<ref name=Mv/>
| absmag_v=16.614<ref name=houdebine2019/>
}}
}}
{{Starbox detail
{{Starbox detail
| age_myr=100–350<ref name=aaa447/>
| mass={{val|0.110|0.003}}<ref name=pineda2021/>
| metal_fe={{nowrap|+0.18 ± 0.17}}<ref name=apj748_2_934/>
| radius={{val|0.144|0.004}}<ref name=pineda2021/>
| gravity=5.5<ref name=aaa439_3/>
| luminosity=0.00106 ± 0.00002<ref name=pineda2021/>
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| mass=0.09<ref name="RECONS"/>
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| radius=0.16<ref name=aaa235_1_2/>
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| rotational_velocity=< 3.0<ref name=apj583/>
| luminosity_bolometric=0.0014
| luminosity_visual=0.00002
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| temperature={{nowrap|2,800 ± 100}}<ref name=aaa447/>
| habitable_inner=0.024<ref name="aaa555_A104"/>&nbsp;[[Astronomical Unit|AU]]
| habitable_inner=0.024<ref name="aaa555_A104"/>&nbsp;[[Astronomical Unit|AU]]
| habitable_outer=0.052<ref name="aaa555_A104"/>&nbsp;AU
| habitable_outer=0.052<ref name="aaa555_A104"/>&nbsp;AU
| gravity=5.5<ref name=aaa439_3/>
⚫
| temperature={{val|2,749|44|41|fmt=commas}}<ref name=pineda2021/>
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| metal_fe=+0.25<ref name=mann2015/>
| rotation={{val|2.704|0.003|ul=d}}<ref name=da2019/>
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| rotational_velocity={{val|2.9|0.8}}<ref name=lafarga2021/>
| age_gyr=0.1-1.5<ref name="Bowens-Rubin2023"/>
}}
}}
{{Starbox catalog
{{Starbox catalog
| names=CN Leonis, CN Leo, [[Gliese-Jahreiss catalogue|GJ]] 406, [[Henry-Lee Giclas|G]] 045-020, [[Luyten Two-Tenths catalogue|LTT]] 12923, LFT 750, [[Luyten Half-Second catalogue|LHS]] 36,<ref name="SIMBAD" /> [[General Catalogue of Trigonometric Parallaxes|GCTP]] 2553.
| names=CN Leonis, CN Leo, [[Gliese-Jahreiss catalogue|GJ]] 406, [[Henry-Lee Giclas|G]] 045-020, [[Luyten Two-Tenths catalogue|LTT]] 12923, LFT 750, [[Luyten Half-Second catalogue|LHS]] 36, [[General Catalogue of Trigonometric Parallaxes|GCTP]] 2553<ref name="SIMBAD" />
}}
}}
{{Starbox reference
{{Starbox reference
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|image={{Location map|100x100|AlternativeMap=Leo_constellation_map.svg
|image={{Location map|100x100|AlternativeMap=Leo_constellation_map.svg
|alt=Wolf 359 is located in the constellation Leo.
|alt=Wolf 359 is located in the constellation Leo.
|caption=Wolf 359 is shown near the ecliptic in the southern region of [[Leo (constellation)|Leo]]|border=infobox|width=320
|caption=Wolf 359 is shown near the ecliptic in the southern region of [[Leo (constellation)|Leo]].|border=infobox|width=320
|label=Wolf 359
|label=Wolf 359
|position=left
|position=left
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{{Starbox end}}
{{Starbox end}}


'''Wolf 359''' is a [[red dwarf]] star located in the constellation [[Leo (constellation)|Leo]], near the [[ecliptic]]. At a distance of approximately 7.9 [[light year]]s from [[Earth]], it has an [[apparent magnitude]] of 13.54 and can only be seen with a large [[telescope]]. Wolf 359 is one of the [[List of nearest stars|nearest stars]] to the [[Sun]]; only the [[Alpha Centauri]] system (including [[Proxima Centauri]]), [[Barnard's Star]], the [[brown dwarf]]s [[Luhman 16]] (WISE 1049-5319), and [[WISE 0855−0714]] are known to be closer. Its proximity to Earth has led to its mention in several [[Stars and planetary systems in fiction#Wolf 359 (CN Leonis)|works of fiction]].
'''Wolf 359''' is a [[red dwarf]] star located in the constellation [[Leo (constellation)|Leo]], near the [[ecliptic]]. At a distance of {{convert|7.86|ly|pc|lk=on|abbr=off}} from [[Earth]], it has an [[apparent magnitude]] of 13.54 and can only be seen with a large [[telescope]]. Wolf 359 is one of the [[List of nearest stars|nearest stars]] to the [[Sun]] with only the [[Alpha Centauri]] system (including [[Proxima Centauri]]), [[Barnard's Star]], and the [[brown dwarf]]s [[Luhman 16]] (WISE 1049-5319) and [[WISE 0855−0714]] known to be closer. Its proximity to Earth has led to its mention in several works of fiction.<ref>{{Cite book |last=Weir |first=Andy |title=Project Hail Mary |date=2022 |publisher=Penguin Books |isbn=978-1-5291-5746-8 |location=London}}</ref>


Wolf 359 is one of the faintest and lowest-mass stars known. At the light-emitting layer called the [[photosphere]], it has a temperature of about 2,800&nbsp;[[Kelvin|K]], which is low enough for [[chemical compound]]s to form and survive. The [[absorption line]]s of compounds such as water and [[titanium(II) oxide]] have been observed in the [[stellar spectrum|spectrum]].<ref name=apj596_1/> The surface has a [[magnetic field]] that is stronger than the average magnetic field on the [[Sun]]. As a result of magnetic activity caused by [[convection zone|convection]], Wolf 359 is a [[flare star]] that can undergo sudden increases in luminosity for several minutes. These flares emit strong bursts of [[X-ray]] and [[gamma ray]] radiation that have been observed by [[space telescope]]s. Wolf 359 is a relatively young star with an age of less than a billion years. Two planetary companions are suspected but as yet no [[debris disk]]s have been unmasked.<ref name=barnes/>
Wolf 359 is one of the faintest and least-massive nearby stars known. At the light-emitting layer called the [[photosphere]], it has a temperature of ~2,800&nbsp;[[Kelvin|K]], low enough for [[chemical compound]]s to form and survive. The [[absorption line]]s of compounds such as water and [[titanium(II) oxide]] have been observed in its [[stellar spectrum|spectrum]].<ref name=apj596_1/> The star's surface has a [[magnetic field]] hundreds of times as strong as that of the [[Sun]], generated by its thorough internal [[Convection zone|convection]]. As a result of this significant magnetic activity, Wolf 359 is a [[flare star]] that can undergo sudden and great increases in luminosity, which can persist for several minutes. These flares emit strong bursts of [[X-ray]] and [[gamma ray]] radiation that have been observed by [[space telescope]]s. It is a relatively young star with an estimated age of less than a billion years. No planetary companions for Wolf 359 have been confirmed so far, though there is one unverified candidate, and as yet no [[debris disk]]s have been found.<ref name="Bowens-Rubin2023"/>


==Observation history and name==
==Observation history and name==
Wolf 359 first came to the attention of astronomers because of the relatively high rate of [[wikt:transverse|transverse]] motion against the background, known as the [[proper motion]]. A high rate of proper motion can indicate that a star is located nearby, as more distant stars must move at higher velocities in order to achieve the same rate of angular travel across the [[celestial sphere]]. The proper motion of Wolf 359 was first measured in 1917 by German [[astronomer]] [[Max Wolf]], with the aid of [[astrophotography]]. In 1919 he published a catalog of over one thousand stars with high [[proper motion]]s, including this one, that are still identified by his name.<ref name=vbsh7_10/> He listed this star as entry number 359, and the star has since been referred to as Wolf 359 in reference to Max Wolf's catalogue.<ref name=an204/>
Wolf 359 first came to the attention of astronomers because of its relatively high rate of [[wikt:transverse|transverse]] motion against the background, also known as the [[proper motion]]. A high rate of proper motion can indicate that the star is located nearby, as closer stars can achieve the same rate of angular change with a lower relative speed. The proper motion of Wolf 359 was first measured in 1917 by German [[astronomer]] [[Max Wolf]], aided by [[astrophotography]]. In 1919 he published a catalogue of over one thousand stars with high [[proper motion]]s, including this one, that are still identified by his name.<ref name=vbsh7_10/> He listed this star as entry number 359, and the star has since been referred to as Wolf 359, in reference to Max Wolf's work.<ref name=an204/>


The first [[parallax]] measurement of Wolf 359 was reported in 1928 from the [[Mount Wilson Observatory]], yielding an annual shift in the star's position of {{nowrap|0.407 ± 0.009 [[arcsecond]]s}}. From this position change, and the known size of the Earth's orbit, the distance to the star could be estimated. It was the lowest-mass and faintest star known until the discovery of [[VB 10]] in 1944.<ref name=cmwo356/><ref name="Biesbroeck"/> The [[infrared]] magnitude of the star was measured in 1957.<ref name=aj62/> In 1969, a brief flare in the luminosity of Wolf 359 was observed, linking it to the class of [[variable star]]s known as [[flare star]]s.<ref name=apj161/>
The first [[parallax]] measurement of Wolf 359 was reported in 1928 from the [[Mount Wilson Observatory]], yielding an annual shift in the star's position of {{nowrap|0.407 ± 0.009 [[arcsecond]]s}}. From this position change, and the known size of the Earth's orbit, the distance to the star could be estimated. It was the faintest and least-massive star known until the discovery of [[VB 10]] in 1944.<ref name=cmwo356/><ref name="Biesbroeck"/> The [[infrared]] magnitude of the star was measured in 1957.<ref name=aj62/> In 1969, a brief flare in the luminosity of Wolf 359 was observed, linking it to a class of [[variable star]]s known as [[flare star]]s.<ref name=apj161/>


==Properties==
==Properties==
[[File:Angular map of fusors around Sol within 9ly (large).png|thumb|upright=1.5|The position of Wolf 359 on a [[Plan position indicator|radar]] map among all stellar objects or [[star system|stellar systems]] within 9 light years (ly) from the map's center, the Sun (Sol). The diamond-shapes are their positions entered according to [[right ascension]] in [[hour angle|hours angle]] (indicated at the edge of the map's reference disc), and according to their [[declination]]. The second mark shows each's distance from Sol, with the [[Concentric objects|concentric]] circles indicating the distance in steps of one ly.]]
Wolf 359 has a [[stellar classification]] of M6,<ref name=todd1994/> although various sources list a spectral class of M5.5,<ref name="aaa466"/> M6.5<ref name=mnras245_3/> or M8.<ref name="apj451"/> Most [[M-type star]]s are [[red dwarf]]s: they are called red because the energy emission of the star reaches a peak in the red and infrared parts of the spectrum.<ref name=jones09/> Wolf 359 has a very low luminosity, emitting about 0.1% of the [[solar luminosity|Sun's energy]].<ref name=aaa447/><ref name=jaavso30_2/> If it were moved to the location of the Sun, it would appear ten times as bright as the [[full Moon]].<ref name=borgia06/>
Wolf 359 has a [[stellar classification]] of M6,<ref name=todd1994/> although various sources list a spectral class of M5.5,<ref name="aaa466"/> M6.5<ref name=mnras245_3/> or M8.<ref name="apj451"/> Most [[M-type star]]s are [[red dwarf]]s: they are visually red because the energy emission of such stars reaches a peak in the red and infrared parts of the spectrum.<ref name=jones09/> Wolf 359 has a very low luminosity, emitting about 0.1% of the [[Solar luminosity|Sun's power]].<ref name=aaa447/><ref name=pineda2021/> If it were moved to the location of the Sun, it would appear ten times as bright as the [[full Moon]].<ref name=borgia06/>


At an estimated 9% of the [[Solar mass|Sun's mass]], Wolf 359 is just above the lowest limit at which a star can perform [[hydrogen fusion]] through the [[proton–proton chain reaction]]: 8% of the Sun's mass.<ref name=apj296/> ([[Substellar object]]s below this limit are known as [[brown dwarf]]s.) The radius of Wolf 359 is an estimated 16% of the [[solar radius|Sun's radius]], or about 110,000&nbsp;km.<ref name=apjl500_L195/> For comparison, the equatorial radius of the planet [[Jupiter]] is 71,492&nbsp;km, which is 65% as large as Wolf 359's.<ref name=nasa10/>
At an estimated 11% of the [[Solar mass|Sun's mass]], Wolf 359 is just above the lower limit at which a star's core can undergo [[hydrogen fusion]] through the [[proton–proton chain reaction]]: ~8% of the solar mass.<ref name=apj296/> ([[Substellar object]]s below this limit are known as [[brown dwarf]]s.) The radius of Wolf 359 is an estimated 14.4% [[Solar radius|that of the Sun]],<ref name=pineda2021/> or about {{val|100,200|ul=km|fmt=commas}}.<ref name=apjl500_L195/> For comparison, the equatorial radius of the planet [[Jupiter]] is {{val|71,490|u=km|fmt=commas}}, making the star a mere 40% wider than the planet.<ref name=nasa10/>


The entire star is undergoing [[Convection zone|convection]], whereby the energy generated at the core is being transported toward the surface by the [[convective]] motion of [[plasma (physics)|plasma]], rather than by transmission through [[Radiation zone|radiation]]. This circulation redistributes any accumulation of helium that is generated through [[stellar nucleosynthesis]] at the core throughout the star.<ref name=cook_jewell95/> This process will allow the star to remain on the [[main sequence]] as a [[hydrogen]] fusing star proportionately longer than a star such as the Sun where helium steadily accumulates at the core. In combination with a lower rate of hydrogen consumption due to its low mass, the convection will allow Wolf 359 to remain a main-sequence star for about eight trillion years.<ref name=adams04/>
The entire star [[Convection zone|undergoes convection]], whereby the energy generated at the core is transported toward the surface by the convective motion of stellar [[plasma (physics)|plasma]], rather than through [[electromagnetic radiation]]. This constant circulation redistributes throughout the star any excess accumulation of helium in the core generated by [[stellar nucleosynthesis]].<ref name=cook_jewell95/> This process allows Wolf 359 to remain on the [[main sequence]] as a [[hydrogen]] fusing star for proportionately longer than one such as the Sun, for which helium steadily accumulates in the core and is not diluted. In conjunction with a much lower rate of hydrogen consumption due to its low mass and core temperature, Wolf 359 is expected to remain a main sequence star for about eight trillion years before finally exhausting its hydrogen supply and ending up as a helium [[white dwarf]].<ref name=adams04/>


A search of this star by the [[Hubble Space Telescope]] revealed no stellar companions, but two candidate planets have since been detected.<ref name=apj119_2/> No [[infrared excess|excess infrared emission]] has been detected, which may indicate the lack of a [[debris disk]] in orbit around it.<ref name=apj667/><ref name=aaa506_3/> [[Radial velocity]] measurements of this star using the Near Infrared Spectrometer (NIRSPEC) instrument at the [[Keck II]] observatory have not revealed any variations that might otherwise indicate the presence of an orbiting companion. This instrumentation is sensitive enough to detect the [[gravitational perturbation]]s of massive, short period companions with the mass of [[Neptune]] or greater.<ref name=aaa538_A141/>
A search of this star by the [[Hubble Space Telescope]] revealed no stellar companions.<ref name=apj119_2/> No [[infrared excess|excess infrared emission]] has been detected, which may indicate the lack of a [[debris disk]] around it.<ref name=apj667/><ref name=aaa506_3/>


===Outer atmosphere===
===Outer atmosphere===
The outer, light-emitting layer of a star is known as the [[photosphere]]. Temperature estimates of the photosphere of Wolf 359 range from 2,500&nbsp;K to 2,900&nbsp;K,<ref name=mnras389_2/> which is sufficiently cool for [[equilibrium chemistry]] to occur. The resulting [[chemical compound]]s survive long enough to be observed through their [[spectral lines]].<ref name=verschuur03/> Numerous [[Molecule|molecular]] bands appear in the spectrum of Wolf 359, including those of [[carbon monoxide]] (CO),<ref name=aaa396/> [[Iron(I) hydride|iron hydride]] (FeH), [[chromium]] hydride (CrH), water (H<sub>2</sub>O),<ref name=apj596_1/> [[magnesium]] hydride (MgH), [[vanadium(II) oxide]] (VO),<ref name=aaa447/> [[titanium(II) oxide]] (TiO) and possibly the molecule CaOH.<ref name=apj174/> Since there are no lines of [[lithium]] in the spectrum, this element must have already been consumed by fusion at the core. This indicates the star must be at least 100 million years old.<ref name=aaa447/>
The outer, light-emitting layer of a star is known as the [[photosphere]]. Estimates of the photospheric temperature of Wolf 359 range from 2,500&nbsp;K to 2,900&nbsp;K,<ref name=mnras389_2/> which is sufficiently cool for [[equilibrium chemistry]] to occur. The resulting [[chemical compound]]s survive long enough to be observed through their [[spectral lines]].<ref name=verschuur03/> Numerous [[Molecule|molecular]] bands appear in the spectrum of Wolf 359, including those of [[carbon monoxide]] (CO),<ref name=aaa396/> [[Iron(I) hydride|iron hydride]] (FeH), [[Chromium(I) hydride|chromium hydride]] (CrH), [[water]] (H<sub>2</sub>O),<ref name=apj596_1/> [[magnesium]] hydride (MgH), [[vanadium(II) oxide]] (VO),<ref name=aaa447/> [[titanium(II) oxide]] (TiO), and possibly the molecule CaOH.<ref name=apj174/> Since there are no lines of [[lithium]] in the spectrum, this element must have already been consumed by fusion in the core. This indicates that the star must be at least 100 million years old.<ref name=aaa447/>


Beyond the photosphere lies a nebulous, high temperature region known as the [[stellar corona]]. In 2001, Wolf 359 became the first star other than the Sun to have the spectrum of its corona observed from a ground-based telescope. The spectrum showed [[emission line]]s of Fe XIII, which is heavily [[ion]]ized iron that has been stripped of twelve of its electrons.<ref name=nature412_2/> The strength of this line can vary over a time period of several hours, which may be evidence of [[wikt:microflare|microflare]] heating.<ref name=aaa447/>
Beyond the photosphere lies a nebulous, high temperature region known as the [[stellar corona]]. In 2001, Wolf 359 became the first star other than the Sun to have the spectrum of its corona observed by a ground-based telescope. The spectrum showed [[emission line]]s of Fe XIII, which is heavily [[ion]]ized iron that has been stripped of twelve of its twenty-six electrons.<ref name=nature412_2/> The strength of this line can vary over a time period of several hours, which may be evidence of [[wikt:microflare|microflare]] heating.<ref name=aaa447/>


[[File:CNLeoLightCurve.png|thumb|left|A [[Photometric_system#Photometric_letters|blue band]] [[light curve]] for a flare on CN Leonis, adapted from Liefke ''et al.'' (2007)<ref name="Liefke2007"/>]]
[[File:CNLeoLightCurve.png|thumb|left|A [[Photometric system#Photometric letters|blue band]] [[light curve]] for a flare of CN Leonis, adapted from Liefke ''et al.'' (2007)<ref name="Liefke2007"/>]]
Wolf 359 is classified as a [[Luyten 726-8|UV Ceti]]-type [[flare star]],<ref name=ass95_2/> which is a star that undergoes brief, energetic increases in luminosity because of magnetic activity in the photosphere. Its [[variable star designation]] is ''CN Leonis''. Wolf 359 has a relatively high flare rate. Observations with the Hubble Space Telescope detected 32 flare events within a two-hour period, with energies of 10<sup>27</sup> [[erg]]s (10<sup>20</sup> [[joule]]s) and higher.<ref name="apj451"/> The mean magnetic field at the surface of Wolf 359 has a strength of about 2.2&nbsp;[[Gauss (unit)|kG]] (0.22 [[tesla (unit)|teslas]]), but this varies significantly on time scales as short as six hours.<ref name="aaa466"/> By comparison, the magnetic field of the Sun averages 1&nbsp;gauss (100 [[microtesla|μT]]), although it can rise as high as 3&nbsp;kG (0.3 T) in active [[sunspot]] regions.<ref name=noao070107/> During flare activity, Wolf 359 has been observed emitting [[X-ray]]s and [[gamma ray]]s.<ref name=apj450_9/><ref name=appb37_3/>
Wolf 359 is classified as a [[Luyten 726-8|UV Ceti]]-type [[flare star]],<ref name=ass95_2/> a category of stars that undergo brief, dramatic increases in luminosity due to intense magnetic field activity in their photospheres. Its [[variable star designation]] is ''CN Leonis''. Wolf 359 has a relatively high flare rate. Observations with the Hubble Space Telescope detected 32 flare events within a two-hour period, with energies of 10<sup>27</sup> [[erg]]s (10<sup>20</sup> [[joule]]s) and higher.<ref name="apj451"/> The mean magnetic field strength at the surface of the star is around 2.2&nbsp;[[Gauss (unit)|kG]] (0.22 [[tesla (unit)|teslas]]), but this value varies significantly on time scales as short as six hours.<ref name="aaa466"/> In comparison, the magnetic field of the Sun averages a strength of 1&nbsp;gauss (100 [[microtesla|μT]]), although it can reach as high as 3&nbsp;kG (0.3 T) in active [[sunspot]] regions.<ref name=noao070107/> During periods of flare activity, Wolf 359 has been observed to emit [[X-ray]]s and [[gamma ray]]s.<ref name=apj450_9/><ref name=appb37_3/>


===Motion===
===Motion===
[[File:Near-stars-past-future-en.svg|right|thumb|300px|Distances of the [[List of nearest stars|nearest stars]] from 20,000 years ago until 80,000 years in the future. Wolf 359 is not shown, but it currently has a distance of 7.9ly and increasing, with the minimum of 7.3ly at about -13,850 years]]
[[File:Near-stars-past-future-en.svg|right|thumb|300px|Distances of the [[List of nearest stars|nearest stars]] from 20,000 years ago to 80,000 years in the future. Wolf 359 is not displayed, but it is currently at a distance of 7.9&nbsp;ly and increasing, with a past minimum of 7.3&nbsp;ly around 13,850 years ago.]]
The rotation of a star causes a [[Doppler shift]] to the spectrum. On average, this results in a broadening of the [[absorption line]]s in its spectrum, with the lines increasing in width with higher rates of rotation. However, only the rotational motion in the direction of the observer can be measured by this means, so the resulting data provides a lower limit on the star's rotation. This projected [[Stellar rotation|rotational velocity]] of Wolf 359's equator is less than 3&nbsp;km/s, which is below the threshold of detection through [[spectral line broadening]].<ref name=apj583/> This low rate of rotation may have been caused by loss of [[angular momentum]] through a [[stellar wind]]. Typically, the time scale for the spin down of a star at spectral class M6 is roughly 10 billion years, because fully convective stars like this lose their rotation more slowly than other stars.<ref name=roeser08/> However, evolutionary models suggest that Wolf 359 is a relatively young star with an age of less than a billion years.<ref name=aaa447/>
The rotation of a star causes a [[Doppler shift]] of its spectrum, generally resulting in a broadening of the [[absorption line]]s in its spectrum, with the lines increasing in width with higher rotational speeds. However, only the rotational velocity's component in the direction of the observer can be measured by this method, and the resulting data imposes only a lower limit on the star's rotational speed. This projected [[Stellar rotation|rotational velocity]] of Wolf 359 at its equator is less than 3&nbsp;km/s, below the threshold of detection with [[spectral line broadening]].<ref name=apj583/> This low rate of rotation may have been caused by the loss of [[angular momentum]] through its [[stellar wind]], which increases greatly during periods of flare activity. Roughly speaking, the spin-down timescale of a star of spectral class M6 is somewhat long, at ~10 billion years, as fully convective stars lose their rotational speeds more slowly than others.<ref name=roeser08/> However, evolutionary models suggest that Wolf 359 is a relatively young star with an age of less than a billion years.<ref name=aaa447/>


The proper motion Wolf 359 against the background is 4.696&nbsp;[[arcsecond]]s per year, and it is moving away from the Sun at a velocity of 19&nbsp;km/s.<ref name=apj583/><ref name="RECONS"/> When translated into the [[galactic coordinate system]], this motion corresponds to a [[space velocity (astronomy)|space velocity]] of {{nowrap|(U, V, W)}} = {{nowrap|(−26, −44, −18) km/s}}.<ref name=gliese69/> The space velocity of Wolf 359 implies that it belongs to the population of [[old-disk star]]s. It follows an orbit through the [[Milky Way]] that will bring it as close as {{Convert|20.5|kly|kpc|abbr=on}} and as distant as {{Convert|28|kly|kpc|abbr=on}} from the [[Galactic Center]]. The galactic orbit has an [[orbital eccentricity|eccentricity]] of 0.156, and the star can travel as far as {{convert|444|ly|pc}} away from the [[galactic plane]].<ref name=rmaa34/> The closest stellar neighbor to Wolf 359 is the red dwarf [[Ross 128]] at {{Convert|3.79|ly|pc|abbr=on|lk=on}} away.<ref name=solstation/> Approximately 13,850 years ago, Wolf 359 was at its minimal distance of about {{Convert|7.35|ly|pc|abbr=on}} from the Sun.<ref name="SIMBAD2"/>
Wolf 359's proper motion is 4.696&nbsp;[[arcsecond]]s per year, and moving away from the Sun at a velocity of ~19&nbsp;km/s.<ref name=apj583/><ref name="RECONS"/> When translated into the [[galactic coordinate system]], the motion corresponds to a [[space velocity (astronomy)|space velocity]] of {{nowrap|(U, V, W)}} = {{nowrap|(−26, −44, −18) km/s}}.<ref name=gliese69/> This space velocity implies that Wolf 359 belongs to the population of [[old-disk star]]s. It follows an orbit through the [[Milky Way]] that will bring it as close as {{Convert|20.5|kly|kpc|abbr=on}} and as distant as {{Convert|28|kly|kpc|abbr=on}} from the [[Galactic Center]]. The predicted galactic orbit has an [[orbital eccentricity|eccentricity]] of 0.156, and the star can travel as far as {{convert|444|ly|pc}} away from the [[galactic plane]].<ref name=rmaa34/> The closest stellar neighbor to Wolf 359 is the red dwarf [[Ross 128]], at {{Convert|3.79|ly|pc|abbr=on|lk=on}}.<ref name=solstation/> Approximately 13,850 years before the present day, Wolf 359 attained its minimal separation of about {{Convert|7.35|ly|pc|abbr=on}} from the Sun, and has been receding away ever since.<ref name="SIMBAD2"/>


==Search for planets==
==Planetary system==
[[Radial velocity]] measurements of the star in 2011 using the Near Infrared Spectrometer (NIRSPEC) instrument at the [[Keck II]] observatory did not reveal any variations that might otherwise indicate the presence of an orbiting companion. This instrumentation is sensitive enough to detect the [[gravitational perturbation]]s of massive, short period companions with the mass of [[Neptune]] or greater.<ref name=aaa538_A141/>


In June of 2019, an international team of astronomers led by [[Mikko Tuomi]] from the [[University of Hertfordshire]], UK, submitted a paper to a publication for peer-review with the results of the first reported detection of two candidate exoplanets orbiting Wolf 359 using the [[radial velocity method]] from observations with [[HARPS]] in Chile and [[HIRES]] in Hawaii.<ref name=barnes/> The setup of the system is similar to but more extreme than that of nearby red dwarf [[Proxima Centauri]], both having a close-in low-mass planet and a farther out higher-mass planet. The inner planet, Wolf 359c, receives about three times more stellar radiation than Earth does, making it very unlikely to be a habitable planet.<ref name="barnes"/>
In June 2019, an international team of astronomers led by [[Mikko Tuomi]] from the [[University of Hertfordshire]], UK, submitted a [[preprint]] with the results of the first reported detection of two candidate exoplanets orbiting Wolf 359 using the [[radial velocity method]] from observations with [[HARPS]] in Chile and [[HIRES]] in Hawaii.<ref name=barnes/> If these planets were confirmed, the setup of the system would be similar to but more extreme than that of the nearby red dwarf [[Proxima Centauri]], with both having a close-in low-mass planet and a farther out higher-mass planet. The theorized and later ruled-out inner planet, Wolf 359 c, would receive per unit area about forty times as much radiative energy as compared to Earth, making it unlikely to be a habitable planet. The as yet unconfimed Wolf 359 b, in contrast, is classified as a cool super-[[Neptune]], receiving roughly a third to a quarter of the energy per unit area as Neptune does from the Sun.<ref name="barnes"/>

Further observations from the [[CARMENES survey]] have found that the radial velocity signal corresponding to the inner planet candidate Wolf 359 c is a false positive, resulting from the rotation of the star rather than a planetary companion.<ref name=lafarga2021/><ref name="Ribas2023"/> A 2023 follow-up study using MAROON-X, CARMENES, HARPS, and HIRES radial velocity data as well as imaging data was unable to either confirm or refute the presence of Wolf 359 b. The same study ruled out the existence of any [[brown dwarf|brown dwarfs]] or massive gas giant companions within 10 [[Astronomical unit|AU]] of the star, planets more than half the mass of Jupiter within 1 AU, and planets more massive than [[Uranus]] within 0.1 AU.<ref name="Bowens-Rubin2023"/>


{{OrbitboxPlanet begin}}
{{OrbitboxPlanet begin}}
{{OrbitboxPlanet
{{OrbitboxPlanet hypothetical
| exoplanet = c
| mass_earth = {{val|3.8|2.0|1.6}}
| period = {{val|2.68687|0.00039|0.00031}}
| semimajor = {{val|0.018|0.002}}
| eccentricity = {{val|0.15|0.20|0.15}}
| inclination =
}}
{{OrbitboxPlanet
| exoplanet = b
| exoplanet = b
| mass_earth = {{val|43.9|29.5|23.9}}
| mass_earth = {{val|43.9|29.5|23.9|p=≥}}
| period = {{val|2938|436|fmt=commas}}
| period = {{val|2938|436|fmt=commas}}
| semimajor = {{val|1.845|0.289|0.258}}
| semimajor = {{val|1.845|0.289|0.258}}
Line 124: Line 122:
* [[List of brown dwarfs]]
* [[List of brown dwarfs]]
* [[List of nearest stars and brown dwarfs]]
* [[List of nearest stars and brown dwarfs]]
* [[Stars and planetary systems in fiction#Wolf 359 (CN Leonis)|Wolf 359 in fiction]]


==References==
==References==
{{reflist|colwidth=30em|refs=
{{reflist|colwidth=30em|refs=


<ref name=dr3>{{cite Gaia DR3|3864972938605115520}}</ref>
⚫
<ref name="Liefke2007">{{cite journal |last1=Liefke |first1=C. |last2=Reiners |first2=A. |last3=Schmitt |first3=J. H. M. M. |title=Magnetic field variations and a giant flare Multiwavelength observations of CN Leo |journal=Memorie della Societa Astronomica Italiana |date=January 2007 |volume=78 |pages=258-260 |url=https://ui.adsabs.harvard.edu/abs/2007MmSAI..78..258L |access-date=17 January 2022}}</ref>

<ref name="pineda2021">{{cite journal
| title=The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars
| last1=Pineda | first1=J. Sebastian | last2=Youngblood | first2=Allison
| last3=France | first3=Kevin
| journal=The Astrophysical Journal
| volume=918 | issue=1 | id=40 | pages=23 | date=September 2021
| doi=10.3847/1538-4357/ac0aea | arxiv=2106.07656
| bibcode=2021ApJ...918...40P | s2cid=235435757 | doi-access=free }}</ref>


⚫
<ref name="Liefke2007">{{cite journal |last1=Liefke |first1=C. |last2=Reiners |first2=A. |last3=Schmitt |first3=J. H. M. M. |title=Magnetic field variations and a giant flare Multiwavelength observations of CN Leo |journal=Memorie della Societa Astronomica Italiana |date=January 2007 |volume=78 |pages=258–260 |bibcode=2007MmSAI..78..258L }}</ref>
<ref name=Mv>Assuming negligible [[Extinction (astronomy)|extinction]] at this distance, the absolute magnitude ''M'' is determined as follows:
:{| style="border-collapse:collapse; white-space:nowrap;"
| ''M'' || = ''m'' – 5(log<sub>10</sub>( ''D'' ) – 1)
|-
| || = 13.54 – 5(log<sub>10</sub>( 2.39 ) – 1)
|-
| || = 13.54 – 5(0.378 – 1) = 16.65
|}
where ''m'' is the apparent magnitude, ''D'' is the distance in parsecs and log<sub>10</sub> is the base-10 [[logarithm]]. See:<br>
:{{cite book | first=Kenneth R. | last=Lang | date=2006 | title=Astrophysical formulae | series=Astronomy and Astrophysics Library | page=31 | volume=1 | edition=3rd | publisher=Birkhäuser | isbn=978-3-540-29692-8}}</ref>


<ref name="SIMBAD">{{cite web | title=V* CN Leo -- Flare Star | work=SIMBAD | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=Wolf+359 | access-date=2007-07-16 }}</ref>
<ref name="SIMBAD">{{cite web | title=V* CN Leo -- Flare Star | work=SIMBAD | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=Wolf+359 | access-date=2007-07-16 }}</ref>


<ref name=barnes>{{Cite arXiv|eprint=1906.04644v1|last1=Tuomi|first1=M.|title=Frequency of planets orbiting M dwarfs in the Solar neighbourhood|last2=Jones|first2=H. R. A.|last3=Anglada-Escudé|first3=G.|last4=Butler|first4=R. P.|last5=Arriagada|first5=P.|last6=Vogt|first6=S. S.|last7=Burt|first7=J.|last8=Laughlin|first8=G.|last9=Holden|first9=B.|last10=Teske|first10=J. K.|last11=Shectman|first11=S. A.|last12=Crane|first12=J. D.|last13=Thompson|first13=I.|last14=Keiser|first14=S.|last15=Jenkins|first15=J. S.|last16=Berdiñas|first16=Z.|last17=Diaz|first17=M.|last18=Kiraga|first18=M.|last19=Barnes|first19=J. R.|class=astro-ph.EP|year=2019}}</ref>
<ref name=barnes>{{Cite arXiv|eprint=1906.04644 |last1=Tuomi|first1=M.|title=Frequency of planets orbiting M dwarfs in the Solar neighbourhood|last2=Jones|first2=H. R. A.|last3=Anglada-Escudé|first3=G.|last4=Butler|first4=R. P.|last5=Arriagada|first5=P.|last6=Vogt|first6=S. S.|last7=Burt|first7=J.|last8=Laughlin|first8=G.|last9=Holden|first9=B.|last10=Teske|first10=J. K.|last11=Shectman|first11=S. A.|last12=Crane|first12=J. D.|last13=Thompson|first13=I.|last14=Keiser|first14=S.|last15=Jenkins|first15=J. S.|last16=Berdiñas|first16=Z.|last17=Diaz|first17=M.|last18=Kiraga|first18=M.|last19=Barnes|first19=J. R.|class=astro-ph.EP|year=2019}}</ref>


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Line 151: Line 148:


<ref name="RECONS">{{cite web | author=Staff | date=June 8, 2007 | url=http://joy.chara.gsu.edu/RECONS/ | title=List of the nearest 100 stellar systems | publisher=Research Consortium on Nearby Stars | access-date=2007-07-16 }}</ref>
<ref name="RECONS">{{cite web | author=Staff | date=June 8, 2007 | url=http://joy.chara.gsu.edu/RECONS/ | title=List of the nearest 100 stellar systems | publisher=Research Consortium on Nearby Stars | access-date=2007-07-16 }}</ref>

<ref name=aaa235_1_2>{{cite journal | display-authors=1 | last1=Doyle | first1=J. G. | last2=Butler | first2=C. J. | title=Optical and infrared photometry of dwarf M and K stars | journal=Astronomy and Astrophysics | date=1990 | volume=235 | issue=1–2 | pages=335–339 | bibcode=1990A&A...235..335D }}</ref>


<ref name=apj583>{{cite journal | display-authors=1 | last1=Mohanty | first1=Subhanjoy | last2=Basri | first2=Gibor | title=Rotation and activity in mid-M to L field dwarfs | journal=The Astrophysical Journal | date=2003 | volume=583 | issue=1 | pages=451–472 | bibcode=2003ApJ...583..451M | doi=10.1086/345097 |arxiv = astro-ph/0201455 | s2cid=119463177 }}</ref>
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<ref name=jaavso30_2>{{cite journal | last=West | first=Frederick R. | title=Letter to the Editor: the corona of CN Leonis (Gliese 406) and its possible detection at radio frequencies | journal=The Journal of the American Association of Variable Star Observers | date=2002 | volume=30 | issue=2 | pages=149–150 | bibcode=2002JAVSO..30..149W }}</ref>


<ref name=an204>{{cite journal | title=Eigenbewegungssterne | last1=Wolf | first1=M. | journal=Astronomische Nachrichten | volume=204 | issue=20 | pages=345–350 |date=July 1917 | bibcode=1917AN....204..345W | doi=10.1002/asna.19172042002}}</ref>
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Line 170: Line 163:
<ref name="SIMBAD2">{{cite web | url=http://cdsannotations.u-strasbg.fr/annotations/simbadObject/1769389 | work=SIMBAD | title=Annotations on V* CN Leo object | publisher=Centre de Données astronomiques de Strasbourg | access-date=2010-04-13 }}</ref>
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<ref name=apj596_1>{{cite journal | display-authors=1 | last1=McLean | first1=Ian S. | last2=McGovern | first2=Mark R. | last3=Burgasser | first3=Adam J. | last4=Kirkpatrick | first4=J. Davy | last5=Prato | first5=L. | last6=Kim | first6=Sungsoo S. | title=The NIRSPEC brown dwarf spectroscopic survey. I. low-resolution near-infrared spectra | doi=10.1086/377636 | journal=The Astrophysical Journal | volume=596 | issue=1 | pages=561–586 |date=October 2003 | bibcode=2003ApJ...596..561M|arxiv = astro-ph/0309257 | s2cid=1939667 }}</ref>
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<ref name=apj174>{{cite journal | last1=Pesch | first1=Peter |date=June 1972 | title=CaOH, a new triatomic molecule in stellar atmospheres | journal=Astrophysical Journal | volume=174 | doi=10.1086/180970 | pages=L155 | bibcode=1972ApJ...174L.155P}}</ref>
<ref name=apj174>{{cite journal | last1=Pesch | first1=Peter |date=June 1972 | title=CaOH, a new triatomic molecule in stellar atmospheres | journal=Astrophysical Journal | volume=174 | doi=10.1086/180970 | pages=L155 | bibcode=1972ApJ...174L.155P| doi-access=free }}</ref>


<ref name=nature412_2>{{cite journal | display-authors=1 | last1=Schmitt | first1=J. H. M. M. | last2=Wichmann | first2=R. | title=Ground-based observation of emission lines from the corona of a red-dwarf star | journal=Nature | date=2001 | volume=412 | issue=2 | pages=508–510 | doi=10.1038/35087513 | pmid=11484044 | bibcode=2001Natur.412..508S | s2cid=4415051 }}</ref>
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Line 184: Line 177:
<ref name="apj451">{{cite journal | display-authors=1 | last1=Robinson | first1=R. D. | last2=Carpenter | first2=K. G. | last3=Percival | first3=J. W. | last4=Bookbinder | first4=J. A. | title=A search for microflaring activity on dMe flare stars. I. Observations of the dM8e Star CN Leonis | journal=Astrophysical Journal | date=1995 | volume=451 | pages=795–805 | bibcode=1995ApJ...451..795R | doi=10.1086/176266 }}</ref>
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<ref name=noao070107>{{cite news | author=Staff | date=January 7, 2007 | title=Calling Dr. Frankenstein! : interactive binaries show signs of induced hyperactivity | publisher=National Optical Astronomy Observatory | url=http://www.noao.edu/outreach/press/pr07/pr0701.html | access-date=2006-05-24 }}</ref>
<ref name=noao070107>{{cite news | author=Staff | date=January 7, 2007 | title=Calling Dr. Frankenstein! : interactive binaries show signs of induced hyperactivity | publisher=National Optical Astronomy Observatory }}</ref>


<ref name=apj450_9>{{cite journal | display-authors=1 | last1=Schmitt | first1=J. H. M. M. | last2=Fleming | first2=T. A. | last3=Giampapa | first3=M. S. | title=The X-ray view of the low-mass stars in the solar neighborhood | journal=Astrophysical Journal |date=September 1995 | volume=450 | issue=9 | pages=392–400 | bibcode=1995ApJ...450..392S | doi=10.1086/176149 }}</ref>
<ref name=apj450_9>{{cite journal | display-authors=1 | last1=Schmitt | first1=J. H. M. M. | last2=Fleming | first2=T. A. | last3=Giampapa | first3=M. S. | title=The X-ray view of the low-mass stars in the solar neighborhood | journal=Astrophysical Journal |date=September 1995 | volume=450 | issue=9 | pages=392–400 | bibcode=1995ApJ...450..392S | doi=10.1086/176149 | doi-access=free }}</ref>


<ref name=apj119_2>{{cite journal | display-authors=1 | last1=Schroeder | first1=Daniel J. | last2=Golimowski | first2=David A. | last3=Brukardt | first3=Ryan A. | last4=Burrows | first4=Christopher J. | last5=Caldwell | first5=John J. | last6=Fastie | first6=William G. | last7=Ford | first7=Holland C. | last8=Hesman | first8=Brigette | last9=Kletskin | first9=Ilona | title=A search for faint companions to nearby stars using the wide field planetary camera 2 | journal=The Astronomical Journal | date=2000 | volume=119 | issue=2 | pages=906–922 | bibcode=2000AJ....119..906S | doi=10.1086/301227 | doi-access=free }}</ref>
<ref name=apj119_2>{{cite journal | display-authors=1 | last1=Schroeder | first1=Daniel J. | last2=Golimowski | first2=David A. | last3=Brukardt | first3=Ryan A. | last4=Burrows | first4=Christopher J. | last5=Caldwell | first5=John J. | last6=Fastie | first6=William G. | last7=Ford | first7=Holland C. | last8=Hesman | first8=Brigette | last9=Kletskin | first9=Ilona | title=A search for faint companions to nearby stars using the wide field planetary camera 2 | journal=The Astronomical Journal | date=2000 | volume=119 | issue=2 | pages=906–922 | bibcode=2000AJ....119..906S | doi=10.1086/301227 | doi-access=free }}</ref>
Line 200: Line 193:
<ref name=aj137_5>{{cite journal | last1=Landolt | first1=Arlo U. |date=May 2009 | title=UBVRI photometric standard stars around the celestial equator: Updates and Additions | journal=The Astronomical Journal | volume=137 | issue=5 | pages=4186–4269 | doi=10.1088/0004-6256/137/5/4186 | bibcode=2009AJ....137.4186L |arxiv = 0904.0638 | s2cid=118627330 }} See table II.</ref>
<ref name=aj137_5>{{cite journal | last1=Landolt | first1=Arlo U. |date=May 2009 | title=UBVRI photometric standard stars around the celestial equator: Updates and Additions | journal=The Astronomical Journal | volume=137 | issue=5 | pages=4186–4269 | doi=10.1088/0004-6256/137/5/4186 | bibcode=2009AJ....137.4186L |arxiv = 0904.0638 | s2cid=118627330 }} See table II.</ref>


<ref name=mnras389_2>{{cite journal | display-authors=1 | last1=Casagrande | first1=Luca | last2=Flynn | first2=Chris | last3=Bessell | first3=Michael | title=M dwarfs: effective temperatures, radii and metallicities | journal=Monthly Notices of the Royal Astronomical Society | volume=389 | issue=2 | pages=585–607 |date=September 2008 | doi=10.1111/j.1365-2966.2008.13573.x | bibcode=2008MNRAS.389..585C |arxiv = 0806.2471 | s2cid=14353142 }}</ref>
<ref name=mnras389_2>{{cite journal | display-authors=1 | last1=Casagrande | first1=Luca | last2=Flynn | first2=Chris | last3=Bessell | first3=Michael | title=M dwarfs: effective temperatures, radii and metallicities | journal=Monthly Notices of the Royal Astronomical Society | volume=389 | issue=2 | pages=585–607 |date=September 2008 | doi=10.1111/j.1365-2966.2008.13573.x | doi-access=free | bibcode=2008MNRAS.389..585C |arxiv = 0806.2471 | s2cid=14353142 }}</ref>


<ref name=cook_jewell95>{{cite web | display-authors=1 | last1=McCook | first1=G. P. | last2=Jewell | first2=E. R. | date=1995 | title=Fully convective M dwarfs | publisher=Villanova University | url=http://www.csc.villanova.edu/~astronom/obs95/node12.html | access-date=2010-05-17 | url-status=dead | archive-url=https://web.archive.org/web/20110615064340/http://www.csc.villanova.edu/~astronom/obs95/node12.html | archive-date=2011-06-15 }}</ref>
<ref name=cook_jewell95>{{cite web | display-authors=1 | last1=McCook | first1=G. P. | last2=Jewell | first2=E. R. | date=1995 | title=Fully convective M dwarfs | publisher=Villanova University | url=http://www.csc.villanova.edu/~astronom/obs95/node12.html | access-date=2010-05-17 | url-status=dead | archive-url=https://web.archive.org/web/20110615064340/http://www.csc.villanova.edu/~astronom/obs95/node12.html | archive-date=2011-06-15 }}</ref>


<ref name=apj161>{{cite journal | display-authors=1 | last1=Greenstein | first1=Jesse L. | last2=Neugebauer | first2=G. | last3=Becklin | first3=E. E. | title=The faint end of the main sequence | journal=Astrophysical Journal | volume=161 | pages=519 |date=August 1970 | doi=10.1086/150556 | bibcode=1970ApJ...161..519G | url=https://authors.library.caltech.edu/74718/1/1970ApJ___161__519G.pdf }}</ref>
<ref name=apj161>{{cite journal | display-authors=1 | last1=Greenstein | first1=Jesse L. | last2=Neugebauer | first2=G. | last3=Becklin | first3=E. E. | title=The faint end of the main sequence | journal=Astrophysical Journal | volume=161 | pages=519 |date=August 1970 | doi=10.1086/150556 | bibcode=1970ApJ...161..519G | url=https://resolver.caltech.edu/CaltechAUTHORS:20170303-142748800 }}</ref>


<ref name=adams04>{{cite conference | display-authors=1 | last1=Adams | first1=Fred C. | last2=Laughlin | first2=Gregory | last3=Graves | first3=Genevieve J. M. | title=Red dwarfs and the end of the main sequence | book-title=Gravitational Collapse: From Massive Stars to Planets | pages=46–49 |date=December 2004 | publisher=Revista Mexicana de Astronomía y Astrofísica | bibcode=2004RMxAC..22...46A }}</ref>
<ref name=adams04>{{cite conference | display-authors=1 | last1=Adams | first1=Fred C. | last2=Laughlin | first2=Gregory | last3=Graves | first3=Genevieve J. M. | title=Red dwarfs and the end of the main sequence | book-title=Gravitational Collapse: From Massive Stars to Planets | pages=46–49 |date=December 2004 | publisher=Revista Mexicana de Astronomía y Astrofísica | bibcode=2004RMxAC..22...46A }}</ref>
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<ref name=appb37_3>{{cite journal | display-authors=1 | last1=Cwiok | first1=M. | last2=Czyrkowski | first2=H. | last3=Dabrowski | first3=R. | last4=Dominik | first4=W. | last5=Kasprowicz | first5=G. | last6=Kwiecinska | first6=K. | last7=Malek | first7=K. | last8=Mankiewicz | first8=L. | last9=Molak | first9=M. | title=Search for optical counterparts of gamma ray burst | journal=Acta Physica Polonica B | volume=37 | issue=3 | page=919 |date=March 2006 | bibcode=2006AcPPB..37..919C }}</ref>
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<ref name=rmaa34>{{cite journal | display-authors=1 | last1=Allen | first1=C. | last2=Herrera | first2=M. A. | title=The galactic orbits of nearby UV Ceti stars | journal=Revista Mexicana de Astronomía y Astrofísica | date=1998 | volume=34 | pages=37–46 | bibcode=1998RMxAA..34...37A }}</ref>
<ref name=rmaa34>{{cite journal | display-authors=1 | last1=Allen | first1=C. |author1-link=Christine Allen (astronomer)| last2=Herrera | first2=M. A. | title=The galactic orbits of nearby UV Ceti stars | journal=Revista Mexicana de Astronomía y Astrofísica | date=1998 | volume=34 | pages=37–46 | bibcode=1998RMxAA..34...37A }}</ref>


<ref name=apj296>{{cite journal | display-authors=1 | last1=Dantona | first1=F. | last2=Mazzitelli | first2=I. | title=Evolution of very low mass stars and brown dwarfs. I - The minimum main-sequence mass and luminosity | journal=Astrophysical Journal, Part 1 | volume=296 | date=September 15, 1985 | pages=502–513 | doi=10.1086/163470 | bibcode=1985ApJ...296..502D }}</ref>
<ref name=apj296>{{cite journal | display-authors=1 | last1=Dantona | first1=F. | last2=Mazzitelli | first2=I. | title=Evolution of very low mass stars and brown dwarfs. I - The minimum main-sequence mass and luminosity | journal=Astrophysical Journal, Part 1 | volume=296 | date=September 15, 1985 | pages=502–513 | doi=10.1086/163470 | bibcode=1985ApJ...296..502D | doi-access=free }}</ref>


<ref name=gliese69>{{cite journal | last1=Gliese | first1=W. | title=Catalogue of nearby stars | date=1969 | journal=Veröffentlichungen des Astronomischen Rechen-Instituts Heidelberg | volume=22 | pages=1 | bibcode=1969VeARI..22....1G }}</ref>
<ref name=gliese69>{{cite journal | last1=Gliese | first1=W. | title=Catalogue of nearby stars | date=1969 | journal=Veröffentlichungen des Astronomischen Rechen-Instituts Heidelberg | volume=22 | pages=1 | bibcode=1969VeARI..22....1G }}</ref>
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<ref name=aaa538_A141>{{cite journal | display-authors=1 | last1=Rodler | first1=F. | last2=Deshpande | first2=R. | last3=Zapatero Osorio | first3=M. R. | last4=Martín | first4=E. L. | last5=Montgomery | first5=M. M. | last6=Del Burgo | first6=C. | last7=Creevey | first7=O. L. | title=Search for radial velocity variations in eight M-dwarfs with NIRSPEC/Keck II | journal=Astronomy & Astrophysics | volume=538 | page=A141 |date=February 2012 | doi=10.1051/0004-6361/201117577 | bibcode=2012A&A...538A.141R | arxiv=1112.1382 | s2cid=56103966 }}</ref>
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<ref name="aaa555_A104">{{cite journal | display-authors=1
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| last1=Cantrell | first1=Justin R. | last2=Henry
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| first2=Todd J. | last3=White | first3=Russel J
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| journal=The Astronomical Journal | volume=146 | issue=4 | page=99
| journal=The Astronomical Journal | volume=146 | issue=4 | page=99
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| date=October 2013 | doi=10.1088/0004-6256/146/4/99
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<ref name=todd1994>{{cite journal
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| journal=[[The Astronomical Journal]] | volume=108
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<ref name=2mass>{{cite journal |bibcode=2003yCat.2246....0C |title=VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) |journal=CDS/ADC Collection of Electronic Catalogues |pages=II/246 |volume=2246 |last1=Cutri |first1=Roc M. |last2=Skrutskie |first2=Michael F. |last3=Van Dyk |first3=Schuyler D. |last4=Beichman |first4=Charles A. |last5=Carpenter |first5=John M. |last6=Chester |first6=Thomas |last7=Cambresy |first7=Laurent |last8=Evans |first8=Tracey E. |last9=Fowler |first9=John W. |last10=Gizis |first10=John E. |last11=Howard |first11=Elizabeth V. |last12=Huchra |first12=John P. |last13=Jarrett |first13=Thomas H. |last14=Kopan |first14=Eugene L. |last15=Kirkpatrick |first15=J. Davy |last16=Light |first16=Robert M. |last17=Marsh |first17=Kenneth A. |last18=McCallon |first18=Howard L. |last19=Schneider |first19=Stephen E. |last20=Stiening |first20=Rae |last21=Sykes |first21=Matthew J. |last22=Weinberg |first22=Martin D. |last23=Wheaton |first23=William A. |last24=Wheelock |first24=Sherry L. |last25=Zacarias |first25=N. |year=2003 }}</ref>

<ref name=da2019>{{cite journal |bibcode=2019A&A...621A.126D |title=CARMENES input catalogue of M dwarfs. IV. New rotation periods from photometric time series |last1=Díez Alonso |first1=E. |last2=Caballero |first2=J. A. |last3=Montes |first3=D. |last4=De Cos Juez |first4=F. J. |last5=Dreizler |first5=S. |last6=Dubois |first6=F. |last7=Jeffers |first7=S. V. |last8=Lalitha |first8=S. |last9=Naves |first9=R. |last10=Reiners |first10=A. |last11=Ribas |first11=I. |last12=Vanaverbeke |first12=S. |last13=Amado |first13=P. J. |last14=Béjar |first14=V. J. S. |last15=Cortés-Contreras |first15=M. |last16=Herrero |first16=E. |last17=Hidalgo |first17=D. |last18=Kürster |first18=M. |last19=Logie |first19=L. |last20=Quirrenbach |first20=A. |last21=Rau |first21=S. |last22=Seifert |first22=W. |last23=Schöfer |first23=P. |last24=Tal-Or |first24=L. |journal=Astronomy and Astrophysics |year=2019 |volume=621 |pages=A126 |doi=10.1051/0004-6361/201833316 |arxiv=1810.03338 |s2cid=111386691 }}</ref>

<ref name=houdebine2019>{{cite journal |bibcode=2019AJ....158...56H |title=The Mass-Activity Relationships in M and K Dwarfs. I. Stellar Parameters of Our Sample of M and K Dwarfs |last1=Houdebine |first1=Éric R. |last2=Mullan |first2=D. J. |last3=Doyle |first3=J. G. |last4=de la Vieuville |first4=Geoffroy |last5=Butler |first5=C. J. |last6=Paletou |first6=F. |journal=The Astronomical Journal |year=2019 |volume=158 |issue=2 |pages=56 |doi=10.3847/1538-3881/ab23fe |arxiv=1905.07921 |s2cid=159041104 |doi-access=free }}</ref>

<ref name=lafarga2021>{{cite journal |bibcode=2021A&A...652A..28L |title=The CARMENES search for exoplanets around M dwarfs. Mapping stellar activity indicators across the M dwarf domain |last1=Lafarga |first1=M. |last2=Ribas |first2=I. |last3=Reiners |first3=A. |last4=Quirrenbach |first4=A. |last5=Amado |first5=P. J. |last6=Caballero |first6=J. A. |last7=Azzaro |first7=M. |last8=Béjar |first8=V. J. S. |last9=Cortés-Contreras |first9=M. |last10=Dreizler |first10=S. |last11=Hatzes |first11=A. P. |last12=Henning |first12=Th. |last13=Jeffers |first13=S. V. |last14=Kaminski |first14=A. |last15=Kürster |first15=M. |last16=Montes |first16=D. |last17=Morales |first17=J. C. |last18=Oshagh |first18=M. |last19=Rodríguez-López |first19=C. |last20=Schöfer |first20=P. |last21=Schweitzer |first21=A. |last22=Zechmeister |first22=M. |journal=Astronomy and Astrophysics |year=2021 |volume=652 |page=652 |doi=10.1051/0004-6361/202140605 |arxiv=2105.13467 |s2cid=235248016 }}</ref>

<ref name=mann2015>{{cite journal
| title=How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius
| display-authors=1 | last1=Mann | first1=Andrew W.
| last2=Feiden | first2=Gregory A. | last3=Gaidos | first3=Eric
| last4=Boyajian | first4=Tabetha | last5=von Braun | first5=Kaspar
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<ref name="Ribas2023">{{cite journal |last1=Ribas |first1=I. |last2=Reiners |first2=A. |display-authors=etal |date=February 2023 |title=The CARMENES search for exoplanets around M dwarfs. Guaranteed time observations Data Release 1 (2016-2020) |journal=[[Astronomy & Astrophysics]] |volume=670 |issue= |pages= |doi=10.1051/0004-6361/202244879 |doi-access=free |arxiv=2302.10528 |bibcode=2023A&A...670A.139R}}</ref>

<ref name="Bowens-Rubin2023">{{cite journal |last1=Bowens-Rubin |first1=Rachel |last2=Akana Murphy |first2=Joseph M. |display-authors=etal |date=December 2023 |title=A Wolf 359 in sheep's clothing: Hunting for substellar companions in the fifth-closest system using combined high-contrast imaging and radial velocity analysis |journal=[[The Astronomical Journal]] |volume=166 |issue=6 |pages=260 |doi=10.3847/1538-3881/ad03e5 |arxiv=2309.03402 |bibcode=2023AJ....166..260B |doi-access=free }}</ref>


}}
}}
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| pages=853–861| s2cid=576604
| pages=853–861| s2cid=576604
}}
}}
* {{cite journal |last1=Dittmann |first1=Jason A. |title=Trigonometric Parallaxes for 1507 Nearby Mid-to-late M Dwarfs |year=2014 |journal=[[The Astrophysical Journal]] |volume=784 | issue=2 | pages=156 |arxiv=1312.3241 |doi=10.1088/0004-637X/784/2/156 |bibcode=2014ApJ...784..156D|last2=Irwin |first2=Jonathan M. |last3=Charbonneau |first3=David |last4=Berta-Thompson |first4=Zachory K. |s2cid=18789867 }} [https://www.cfa.harvard.edu/MEarth/MEarth_Parallaxes.txt Table with parallaxes].
* {{cite journal | display-authors=1 | last1=Henry | first1=Todd J. | last2=Subasavage | first2=John P. | last3=Brown | first3=Misty A. | last4=Beaulieu | first4=Thomas D. | last5=Jao | first5=Wei-Chun | last6=Hambly | first6=Nigel C. | title=The solar neighborhood. X. new nearby stars in the southern sky and accurate photometric distance estimates for red dwarfs | journal=The Astronomical Journal | volume=128 | issue=5 | pages=2460–2473 |date=November 2004 | doi=10.1086/425052 | bibcode=2004AJ....128.2460H |arxiv = astro-ph/0408240 | s2cid=15759789 }}


{{nearest systems|2}}
{{nearest systems|1}}
{{Stars of Leo}}
{{Stars of Leo}}
{{Good article}}
{{Good article}}
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[[Category:Wolf objects|0359]]
[[Category:Wolf objects|0359]]
[[Category:Gliese and GJ objects|0406]]
[[Category:Gliese and GJ objects|0406]]
[[Category:Planetary systems with two confirmed planets]]
[[Category:Hypothetical planetary systems]]
[[Category:TIC objects]]
[[Category:TIC objects|365006789]]

Latest revision as of 02:43, 26 October 2024

This article is about the star. For the fictional battle, see The Best of Both Worlds (Star Trek: The Next Generation). For The Outer Limits episode, see Wolf 359 (The Outer Limits). For the podcast, see Wolf 359 (podcast).
Wolf 359

Wolf 359 is the orange-hued star located just above the center of this 2009 astrophotograph.
Observation data
Epoch J2000      Equinox J2000
Constellation Leo
Right ascension 10h 56m 28.92087s[1]
Declination +07° 00′ 53.0033″[1]
Apparent magnitude (V) 13.507[2]
Characteristics
Spectral type M6V[3]
Apparent magnitude (J) 7.1[4]
Apparent magnitude (K) 6.1[4]
U−B color index +1.165[2]
B−V color index +2.034[2]
Variable type UV Ceti[5]
Astrometry
Radial velocity (Rv)+19±1[6] km/s
Proper motion (μ) RA: −3,866.338 mas/yr[1]
Dec.: −2,699.215 mas/yr[1]
Parallax (π)415.1794 ± 0.0684 mas[1]
Distance7.856 ± 0.001 ly
(2.4086 ± 0.0004 pc)
Absolute magnitude (MV)16.614[7]
Details
Mass0.110±0.003[8] M☉
Radius0.144±0.004[8] R☉
Luminosity0.00106 ± 0.00002[8] L☉
Habitable zone inner limit0.024[9] AU
Habitable zone outer limit0.052[9] AU
Surface gravity (log g)5.5[10] cgs
Temperature2,749+44
−41[8] K
Metallicity [Fe/H]+0.25[11] dex
Rotation2.704±0.003 d[12]
Rotational velocity (v sin i)2.9±0.8[13] km/s
Age0.1-1.5[14] Gyr
Other designations
CN Leonis, CN Leo, GJ 406, G 045-020, LTT 12923, LFT 750, LHS 36, GCTP 2553[15]
Database references
SIMBADdata
Wolf 359 is located in the constellation Leo.
Wolf 359 is located in the constellation Leo.
Wolf 359
Wolf 359 is shown near the ecliptic in the southern region of Leo.

Wolf 359 is a red dwarf star located in the constellation Leo, near the ecliptic. At a distance of 7.86 light-years (2.41 parsecs) from Earth, it has an apparent magnitude of 13.54 and can only be seen with a large telescope. Wolf 359 is one of the nearest stars to the Sun with only the Alpha Centauri system (including Proxima Centauri), Barnard's Star, and the brown dwarfs Luhman 16 (WISE 1049-5319) and WISE 0855−0714 known to be closer. Its proximity to Earth has led to its mention in several works of fiction.[16]

Wolf 359 is one of the faintest and least-massive nearby stars known. At the light-emitting layer called the photosphere, it has a temperature of ~2,800 K, low enough for chemical compounds to form and survive. The absorption lines of compounds such as water and titanium(II) oxide have been observed in its spectrum.[17] The star's surface has a magnetic field hundreds of times as strong as that of the Sun, generated by its thorough internal convection. As a result of this significant magnetic activity, Wolf 359 is a flare star that can undergo sudden and great increases in luminosity, which can persist for several minutes. These flares emit strong bursts of X-ray and gamma ray radiation that have been observed by space telescopes. It is a relatively young star with an estimated age of less than a billion years. No planetary companions for Wolf 359 have been confirmed so far, though there is one unverified candidate, and as yet no debris disks have been found.[14]

Observation history and name

[edit]

Wolf 359 first came to the attention of astronomers because of its relatively high rate of transverse motion against the background, also known as the proper motion. A high rate of proper motion can indicate that the star is located nearby, as closer stars can achieve the same rate of angular change with a lower relative speed. The proper motion of Wolf 359 was first measured in 1917 by German astronomer Max Wolf, aided by astrophotography. In 1919 he published a catalogue of over one thousand stars with high proper motions, including this one, that are still identified by his name.[18] He listed this star as entry number 359, and the star has since been referred to as Wolf 359, in reference to Max Wolf's work.[19]

The first parallax measurement of Wolf 359 was reported in 1928 from the Mount Wilson Observatory, yielding an annual shift in the star's position of 0.407 ± 0.009 arcseconds. From this position change, and the known size of the Earth's orbit, the distance to the star could be estimated. It was the faintest and least-massive star known until the discovery of VB 10 in 1944.[20][21] The infrared magnitude of the star was measured in 1957.[22] In 1969, a brief flare in the luminosity of Wolf 359 was observed, linking it to a class of variable stars known as flare stars.[23]

Properties

[edit]
The position of Wolf 359 on a radar map among all stellar objects or stellar systems within 9 light years (ly) from the map's center, the Sun (Sol). The diamond-shapes are their positions entered according to right ascension in hours angle (indicated at the edge of the map's reference disc), and according to their declination. The second mark shows each's distance from Sol, with the concentric circles indicating the distance in steps of one ly.

Wolf 359 has a stellar classification of M6,[3] although various sources list a spectral class of M5.5,[24] M6.5[25] or M8.[26] Most M-type stars are red dwarfs: they are visually red because the energy emission of such stars reaches a peak in the red and infrared parts of the spectrum.[27] Wolf 359 has a very low luminosity, emitting about 0.1% of the Sun's power.[28][8] If it were moved to the location of the Sun, it would appear ten times as bright as the full Moon.[29]

At an estimated 11% of the Sun's mass, Wolf 359 is just above the lower limit at which a star's core can undergo hydrogen fusion through the proton–proton chain reaction: ~8% of the solar mass.[30] (Substellar objects below this limit are known as brown dwarfs.) The radius of Wolf 359 is an estimated 14.4% that of the Sun,[8] or about 100,200 km.[31] For comparison, the equatorial radius of the planet Jupiter is 71,490 km, making the star a mere 40% wider than the planet.[32]

The entire star undergoes convection, whereby the energy generated at the core is transported toward the surface by the convective motion of stellar plasma, rather than through electromagnetic radiation. This constant circulation redistributes throughout the star any excess accumulation of helium in the core generated by stellar nucleosynthesis.[33] This process allows Wolf 359 to remain on the main sequence as a hydrogen fusing star for proportionately longer than one such as the Sun, for which helium steadily accumulates in the core and is not diluted. In conjunction with a much lower rate of hydrogen consumption due to its low mass and core temperature, Wolf 359 is expected to remain a main sequence star for about eight trillion years before finally exhausting its hydrogen supply and ending up as a helium white dwarf.[34]

A search of this star by the Hubble Space Telescope revealed no stellar companions.[35] No excess infrared emission has been detected, which may indicate the lack of a debris disk around it.[36][37]

Outer atmosphere

[edit]

The outer, light-emitting layer of a star is known as the photosphere. Estimates of the photospheric temperature of Wolf 359 range from 2,500 K to 2,900 K,[38] which is sufficiently cool for equilibrium chemistry to occur. The resulting chemical compounds survive long enough to be observed through their spectral lines.[39] Numerous molecular bands appear in the spectrum of Wolf 359, including those of carbon monoxide (CO),[40] iron hydride (FeH), chromium hydride (CrH), water (H2O),[17] magnesium hydride (MgH), vanadium(II) oxide (VO),[28] titanium(II) oxide (TiO), and possibly the molecule CaOH.[41] Since there are no lines of lithium in the spectrum, this element must have already been consumed by fusion in the core. This indicates that the star must be at least 100 million years old.[28]

Beyond the photosphere lies a nebulous, high temperature region known as the stellar corona. In 2001, Wolf 359 became the first star other than the Sun to have the spectrum of its corona observed by a ground-based telescope. The spectrum showed emission lines of Fe XIII, which is heavily ionized iron that has been stripped of twelve of its twenty-six electrons.[42] The strength of this line can vary over a time period of several hours, which may be evidence of microflare heating.[28]

A blue band light curve for a flare of CN Leonis, adapted from Liefke et al. (2007)[43]

Wolf 359 is classified as a UV Ceti-type flare star,[5] a category of stars that undergo brief, dramatic increases in luminosity due to intense magnetic field activity in their photospheres. Its variable star designation is CN Leonis. Wolf 359 has a relatively high flare rate. Observations with the Hubble Space Telescope detected 32 flare events within a two-hour period, with energies of 1027 ergs (1020 joules) and higher.[26] The mean magnetic field strength at the surface of the star is around 2.2 kG (0.22 teslas), but this value varies significantly on time scales as short as six hours.[24] In comparison, the magnetic field of the Sun averages a strength of 1 gauss (100 μT), although it can reach as high as 3 kG (0.3 T) in active sunspot regions.[44] During periods of flare activity, Wolf 359 has been observed to emit X-rays and gamma rays.[45][46]

Motion

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Distances of the nearest stars from 20,000 years ago to 80,000 years in the future. Wolf 359 is not displayed, but it is currently at a distance of 7.9 ly and increasing, with a past minimum of 7.3 ly around 13,850 years ago.

The rotation of a star causes a Doppler shift of its spectrum, generally resulting in a broadening of the absorption lines in its spectrum, with the lines increasing in width with higher rotational speeds. However, only the rotational velocity's component in the direction of the observer can be measured by this method, and the resulting data imposes only a lower limit on the star's rotational speed. This projected rotational velocity of Wolf 359 at its equator is less than 3 km/s, below the threshold of detection with spectral line broadening.[6] This low rate of rotation may have been caused by the loss of angular momentum through its stellar wind, which increases greatly during periods of flare activity. Roughly speaking, the spin-down timescale of a star of spectral class M6 is somewhat long, at ~10 billion years, as fully convective stars lose their rotational speeds more slowly than others.[47] However, evolutionary models suggest that Wolf 359 is a relatively young star with an age of less than a billion years.[28]

Wolf 359's proper motion is 4.696 arcseconds per year, and moving away from the Sun at a velocity of ~19 km/s.[6][48] When translated into the galactic coordinate system, the motion corresponds to a space velocity of (U, V, W) = (−26, −44, −18) km/s.[49] This space velocity implies that Wolf 359 belongs to the population of old-disk stars. It follows an orbit through the Milky Way that will bring it as close as 20.5 kly (6.3 kpc) and as distant as 28 kly (8.6 kpc) from the Galactic Center. The predicted galactic orbit has an eccentricity of 0.156, and the star can travel as far as 444 light-years (136 pc) away from the galactic plane.[50] The closest stellar neighbor to Wolf 359 is the red dwarf Ross 128, at 3.79 ly (1.16 pc).[51] Approximately 13,850 years before the present day, Wolf 359 attained its minimal separation of about 7.35 ly (2.25 pc) from the Sun, and has been receding away ever since.[52]

Search for planets

[edit]

Radial velocity measurements of the star in 2011 using the Near Infrared Spectrometer (NIRSPEC) instrument at the Keck II observatory did not reveal any variations that might otherwise indicate the presence of an orbiting companion. This instrumentation is sensitive enough to detect the gravitational perturbations of massive, short period companions with the mass of Neptune or greater.[53]

In June 2019, an international team of astronomers led by Mikko Tuomi from the University of Hertfordshire, UK, submitted a preprint with the results of the first reported detection of two candidate exoplanets orbiting Wolf 359 using the radial velocity method from observations with HARPS in Chile and HIRES in Hawaii.[54] If these planets were confirmed, the setup of the system would be similar to but more extreme than that of the nearby red dwarf Proxima Centauri, with both having a close-in low-mass planet and a farther out higher-mass planet. The theorized and later ruled-out inner planet, Wolf 359 c, would receive per unit area about forty times as much radiative energy as compared to Earth, making it unlikely to be a habitable planet. The as yet unconfimed Wolf 359 b, in contrast, is classified as a cool super-Neptune, receiving roughly a third to a quarter of the energy per unit area as Neptune does from the Sun.[54]

Further observations from the CARMENES survey have found that the radial velocity signal corresponding to the inner planet candidate Wolf 359 c is a false positive, resulting from the rotation of the star rather than a planetary companion.[13][55] A 2023 follow-up study using MAROON-X, CARMENES, HARPS, and HIRES radial velocity data as well as imaging data was unable to either confirm or refute the presence of Wolf 359 b. The same study ruled out the existence of any brown dwarfs or massive gas giant companions within 10 AU of the star, planets more than half the mass of Jupiter within 1 AU, and planets more massive than Uranus within 0.1 AU.[14]

The Wolf 359 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b (unconfirmed) ≥43.9+29.5
−23.9 M🜨 		1.845+0.289
−0.258 		2,938±436 0.04+0.27
−0.04 		— —

See also

[edit]

References

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