View source for Wolf 359

{{short description|Red dwarf in the constellation Leo}}
{{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)}}
{{Sky|10|56|28.99|+|07|00|52|7.78}}
{{Starbox begin
| name=Wolf 359
}}
{{Starbox image
|image=[[File:Wolf359.jpg|320px]]
|caption=Wolf 359 is the orange-hued star located just above the center of this 2009 [[astrophotograph]].
}}
{{Starbox observe
| epoch=J2000
| constell=[[Leo (constellation)|Leo]]
| ra={{RA|10|56|28.92087}}<ref name=dr3/>
| dec={{DEC|+07|00|53.0033}}<ref name=dr3/>
| appmag_v=13.507<ref name=aj137_5/>
}}
{{Starbox character
| class=M6V<ref name=todd1994/>
| b-v=+2.034<ref name=aj137_5/>
| u-b=+1.165<ref name=aj137_5/>
| variable=[[Flare star|UV Ceti]]<ref name=ass95_2/>
| appmag_1_passband=J
| appmag_1=7.1<ref name=2mass/>
| appmag_2_passband=K
| appmag_2=6.1<ref name=2mass/>
}}
{{Starbox astrometry
| radial_v={{val|+19|1}}<ref name=apj583/>
| prop_mo_ra={{val|-3866.338|fmt=commas}}
| prop_mo_dec={{val|-2699.215|fmt=commas}}
| pm_footnote=<ref name=dr3/>
| parallax=415.1794
| p_error=0.0684
| parallax_footnote=<ref name=dr3/>
| absmag_v=16.614<ref name=houdebine2019/>
}}
{{Starbox detail
| mass={{val|0.110|0.003}}<ref name=pineda2021/>
| radius={{val|0.144|0.004}}<ref name=pineda2021/>
| luminosity=0.00106 ± 0.00002<ref name=pineda2021/>
| habitable_inner=0.024<ref name="aaa555_A104"/>&nbsp;[[Astronomical Unit|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/>
| metal_fe=+0.25<ref name=mann2015/>
| rotation={{val|2.704|0.003|ul=d}}<ref name=da2019/>
| rotational_velocity={{val|2.9|0.8}}<ref name=lafarga2021/>
| age_gyr=0.1-1.5<ref name="Bowens-Rubin2023"/>
}}
{{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, [[General Catalogue of Trigonometric Parallaxes|GCTP]] 2553<ref name="SIMBAD" />
}}
{{Starbox reference
| Simbad = Wolf+359
}}
{{Starbox image
|image={{Location map|100x100|AlternativeMap=Leo_constellation_map.svg
|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
|label=Wolf 359
|position=left
|lat=3.8
|long=44.1
}}|caption=
}}
{{Starbox end}}

'''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]]; 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]] 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]].{{Citation needed|date=May 2024}}

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==
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 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==
[[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 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 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 [[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.<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===
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]] 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 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 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 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/> 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===
[[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]] 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/>

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==
[[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 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 hypothetical
| exoplanet = b
| mass_earth = {{val|43.9|29.5|23.9|p=≥}}
| period = {{val|2938|436|fmt=commas}}
| semimajor = {{val|1.845|0.289|0.258}}
| eccentricity = {{val|0.04|0.27|0.04}}
| inclination =
}}
{{Orbitbox end}}

==See also==
{{Portal|Star}}
* [[List of brown dwarfs]]
* [[List of nearest stars and brown dwarfs]]
* [[Stars and planetary systems in fiction#Wolf 359 (CN Leonis)|Wolf 359 in fiction]]

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

<ref name=dr3>{{cite Gaia DR3|3864972938605115520}}</ref>

<ref name="pineda2021">{{cite journal
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 | last3=France | first3=Kevin 
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<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="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=1906.04644 |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>

<ref name=aaa447>{{cite journal | display-authors=1 | last1=Pavlenko | first1=Ya. V. | last2=Jones | first2=H. R. A. | last3=Lyubchik | first3=Yu. | last4=Tennyson | first4=J. | last5=Pinfield | first5=D. J. | title=Spectral energy distribution for GJ406 | journal=Astronomy and Astrophysics | date=2006 | volume=447 | issue=2 | pages=709–717 | doi=10.1051/0004-6361:20052979 | bibcode=2006A&A...447..709P |arxiv = astro-ph/0510570 | s2cid=119068354 }}</ref>

<ref name=aaa439_3>{{cite journal | display-authors=1 | last1=Fuhrmeister | first1=B. | last2=Schmitt | first2=J. H. M. M. | last3=Hauschildt | first3=P. H. | title=PHOENIX model chromospheres of mid- to late-type M dwarfs | journal=Astronomy and Astrophysics | volume=439 | issue=3 |date=September 2005 | pages=1137–1148 | doi=10.1051/0004-6361:20042338 | bibcode=2005A&A...439.1137F|arxiv = astro-ph/0505375 | s2cid=16499769 }}</ref>

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<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=cmwo356>{{cite journal | last1=van Maanen | first1=Adriaan | title=The photographic determination of stellar parallaxes with the 60- and 100-inch reflectors. Fifteenth Series | journal=Contributions from the Mount Wilson Observatory | volume=356 | pages=1–27 | date=1928 | bibcode=1928CMWCI.356....1V }}</ref>

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<ref name=solstation>{{cite web | url=http://www.solstation.com/stars/wolf359.htm | title=Wolf 359 | publisher=SolStation Company | access-date=2006-08-10 }}</ref>

<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>

<ref name=mnras245_3>{{cite journal | display-authors=1 | last1=Mukai | first1=K. | last2=Mason | first2=K. O. | last3=Howell | first3=S. B. | last4=Allington-Smith | first4=J. | last5=Callanan | first5=P. J. | last6=Charles | first6=P. A. | last7=Hassall | first7=B. J. M. | last8=Machin | first8=G. | last9=Naylor | first9=T. | title=Spectroscopy of faint, high latitude cataclysmic variable candidates | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=245 | issue=3 | pages=385–391 |date=August 1990 | doi=10.1093/mnras/245.3.385 | bibcode=1990MNRAS.245..385M | doi-access=free }}</ref>

<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>

<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>

<ref name=roeser08>{{cite book | title=Reviews in modern astronomy, cosmic matter | first=Siegfried | last=Röser | date=2008 | pages=49–50, 57 | publisher=Wiley-VCH | isbn=978-3-527-40820-7 }}</ref>

<ref name=ass95_2>{{cite journal | display-authors=1 | last1=Gershberg | first1=R. E. | last2=Shakhovskaia | first2=N. I. | title=Characteristics of activity energetics of the UV Cet-type flare stars | journal=Astrophysics and Space Science | date=1983 | volume=95 | issue=2 | pages=235–253 | bibcode=1983Ap&SS..95..235G | doi=10.1007/BF00653631 | s2cid=122101052 }}</ref>

<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 }}</ref>

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<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>

}}

==External links==
{{commons category}}
* [http://www.daviddarling.info/encyclopedia/enwiki/w/Wolf_359.html The Encyclopedia of Astrobiology, Astronomy, and Spaceflight]
* {{Cite journal
 | last=Reiners | first=Ansgar
 | title=Activity-induced radial velocity jitter in a flaring M dwarf
 | journal=Astronomy and Astrophysics
 | volume=498
 | issue=3
 | date=May 2009
 | doi=10.1051/0004-6361/200810257
 | bibcode=2009A&A...498..853R
 | arxiv=0903.2661
 | 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|1}}
{{Stars of Leo}}
{{Good article}}

{{DEFAULTSORT:Wolf 359}}
[[Category:Leo (constellation)]]
[[Category:Local Bubble]]
[[Category:M-type main-sequence stars]]
[[Category:Flare stars]]
[[Category:Objects with variable star designations|Leonis, CN]]
[[Category:Wolf objects|0359]]
[[Category:Gliese and GJ objects|0406]]
[[Category:Hypothetical planetary systems]]
[[Category:TIC objects|365006789]]