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{{Short description|Red supergiant or hypergiant variable star in the constellation Perseus}}
{{Starbox begin
{{Starbox begin
| name = S Persei
| name = S Persei
Line 15: Line 16:
| ra={{RA|2|22|51.70928}}<ref name=hipparcos/>
| ra={{RA|2|22|51.70928}}<ref name=hipparcos/>
| dec={{DEC|58|31|11.4476}}<ref name=hipparcos/>
| dec={{DEC|58|31|11.4476}}<ref name=hipparcos/>
| appmag_v=9.23<ref name="levesque"/> (7.9 - 12.0<ref name=gcvs/>)
| appmag_v=+9.23<ref name="levesque"/> (7.9 - 12.0<ref name=gcvs/>)
| constell=[[Perseus (constellation)|Perseus]]
| constell=[[Perseus (constellation)|Perseus]]
}}
}}
{{Starbox character
{{Starbox character
| class=M4.5I<ref name=levesque/> (M3Iae - M7<ref name=gcvs/>)
| class=M3 Iae–M7<ref name=gcvs/>
| b-v=2.65<ref name="levesque"/>
| b-v=+2.65<ref name="levesque"/>
| u-b=
| u-b=
| variable=[[Semiregular variable|SRc]]<ref name=gcvs/>
| variable=[[Semiregular variable|SRc]]<ref name=gcvs/>
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{{Starbox astrometry
{{Starbox astrometry
| radial_v=-39.71<ref name=famaey/>
| radial_v=-39.71<ref name=famaey/>
| prop_mo_ra=&minus;0.49 ± 0.23<ref name=asaki/>
| prop_mo_ra=–0.49 ± 0.23<ref name=asaki/>
| prop_mo_dec={{nowrap|&minus;1.19 ± 0.20<ref name=asaki/>}}
| prop_mo_dec={{nowrap|&minus;1.19 ± 0.20<ref name=asaki/>}}
| parallax=0.413
| parallax=0.413
| p_error=0.017
| p_error=0.017
| parallax_footnote=<ref name=asaki/>
| parallax_footnote=<ref name=asaki/>
| absmag_v=&minus;6.36 (at m<sub>V</sub> 9.23)<ref name="levesque"/>
| absmag_v=–6.36 (at m<sub>V</sub> 9.23)<ref name="levesque"/>
}}
}}
{{Starbox detail
{{Starbox detail
| mass=20<ref name=yates/>
| mass=20<ref name=yates/>
| radius={{val|1,364|6|fmt=commas}}<ref name="norris">{{Cite thesis|type=PhD|last=Norris|first=Ryan P.|date=2019|title=Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants|url=https://core.ac.uk/download/pdf/225164189.pdf|publisher=[[Georgia State University]]|volume=|pages=|via=}}</ref>
| radius={{val|1,298|64|57|fmt=commas}}<ref name="Norris2023">{{Cite web |last=Norris |first=Ryan |date=2023 |title=Student Science at NMT: Learning Optical Interferometry Through Projects on Evolved Stars |url=https://www.chara.gsu.edu/files/2023Meeting/Norris_NMT_Students_2023.pdf |publisher=[[CHARA array|CHARA]]}}</ref>{{snd}}{{val|1364|6|fmt=commas}}<ref name="norris">{{Cite thesis |last=Norris |first=Ryan |title=Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants |date=2019 |degree=PhD |publisher=[[Georgia State University]] |url=https://scholarworks.gsu.edu/phy_astr_diss/118/ |doi=10.57709/15009706}}</ref>
| luminosity=123,000<ref name=Davies2020>{{Cite journal|last1=Davies|first1=Ben|last2=Beasor|first2=Emma R.|s2cid=210714093|date=March 2020|title=The 'red supergiant problem': the upper luminosity boundary of Type II supernova progenitors|bibcode=2020MNRAS.493..468D|journal=[[MNRAS]]|language=en|volume=493|issue=1|pages=468–476|doi=10.1093/mnras/staa174|arxiv=2001.06020 }}</ref>
| luminosity=123,000<ref name=Davies2020>{{Cite journal|last1=Davies|first1=Ben|last2=Beasor|first2=Emma R.|s2cid=210714093|date=March 2020|title=The 'red supergiant problem': the upper luminosity boundary of Type II supernova progenitors|bibcode=2020MNRAS.493..468D|journal=[[MNRAS]]|language=en|volume=493|issue=1|pages=468–476|doi=10.1093/mnras/staa174|doi-access=free |arxiv=2001.06020 }}</ref> – 186,000<ref name=fok/>
| temperature={{nowrap|3,000<ref name=GarciaHernandez/>–3,500<ref name=michael/>}}
| temperature=3,000<ref name=GarciaHernandez/> – 3,600<ref name=fok/>
| metal=
| metal=
| rotation=
| rotation=
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{{Starbox end}}
{{Starbox end}}


'''S Persei''' is a [[red supergiant]] or [[hypergiant]] located near the [[Double Cluster]] in [[Perseus constellation|Perseus]], north of the cluster [[NGC 869]]. It is a member of the [[Perseus OB1]] [[stellar association|association]] and one of the [[List of largest stars|largest known stars]]. If placed in our solar system, its photospehere would engulf the [[orbit]] of [[Jupiter]]. It is also a [[semiregular variable]], a star whose variations are less regular than those of [[Mira variable]]s.
'''S Persei''' is a [[red supergiant]] or [[hypergiant]] located near the [[Double Cluster]] in [[Perseus constellation|Perseus]], north of the cluster [[NGC 869]]. It is a member of the [[Perseus OB1]] [[stellar association|association]] and one of the [[List of largest stars|largest known stars]]. If placed in the [[Solar System]], its photosphere would engulf the [[orbit]] of [[Jupiter]]. It is also a [[semiregular variable]], a star whose variations are less regular than those of [[Mira variable]]s.


==Discovery==
==Discovery==
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==Variability==
==Variability==
[[File:SPerLightCurve.png|thumb|left|A [[Photometric_system#Photometric_letters|visual band]] [[light curve]] for S&nbsp;Persei, plotted from AAVSO data<ref name="aavso"/>]]
S Persei varies slowly by several [[apparent magnitude|magnitudes]], a factor of over 40 in brightness. It has a main period of somewhat over two years, but shows significant unpredictability. There is a strong variation in the amplitude from around one magnitude to about four magnitudes, and these have been interpreted as [[Beat (acoustics)|beats]] due to a second period of about 940 days.<ref name=smith/> Other analyses find only the primary period of 813 ± 60 days.<ref name=kiss/>
S Persei varies slowly by several [[apparent magnitude|magnitudes]], a factor of over 40 in brightness. It has a main period of somewhat over two years, but shows significant unpredictability. There is a strong variation in the amplitude from around one magnitude to about four magnitudes, and these have been interpreted as [[Beat (acoustics)|beats]] due to a second period of about 940 days.<ref name=smith/> Other analyses find only the primary period of 813 ± 60 days.<ref name=kiss/>


Line 66: Line 68:
Many of the visually bright variable stars belong to this class of semiregulars, as these stars are extremely large and luminous, and hence visible across long distances. S Persei has been described as a [[hypergiant]]<ref name=zhang/> and has a radius over 700 times the sun's radius ({{solar radius|link=y}}).<ref name="levesque"/> Its angular diameter has been measured directly and found to be somewhat elliptical. Modelled as a uniform disk, the radius corresponds to {{solar radius|1,212 ± 124}}.<ref name=thompson/>
Many of the visually bright variable stars belong to this class of semiregulars, as these stars are extremely large and luminous, and hence visible across long distances. S Persei has been described as a [[hypergiant]]<ref name=zhang/> and has a radius over 700 times the sun's radius ({{solar radius|link=y}}).<ref name="levesque"/> Its angular diameter has been measured directly and found to be somewhat elliptical. Modelled as a uniform disk, the radius corresponds to {{solar radius|1,212 ± 124}}.<ref name=thompson/>


The temperature has been calculated from the spectrum using a DUSTY model,<ref name=ivezic/> giving an effective photospheric temperature of 3,500 K and a temperature of 1,000 K for the surrounding dust torus.<ref name=michael>{{cite journal|doi=10.3847/1538-3881/aab961|title=Searching for Cool Dust. II. Infrared Imaging of the OH/IR Supergiants, NML Cyg, VX SGR, S Per, and the Normal Red Supergiants RS per and T per|year=2018|last1=Gordon|first1=Michael S.|last2=Humphreys|first2=Roberta M.|last3=Jones|first3=Terry J.|last4=Shenoy|first4=Dinesh|last5=Gehrz|first5=Robert D.|last6=Helton|first6=L. Andrew|last7=Marengo|first7=Massimo|last8=Hinz|first8=Philip M.|last9=Hoffmann|first9=William F.|s2cid=73650032|journal=The Astronomical Journal|volume=155|issue=5|page=212|arxiv=1708.00018|bibcode=2018AJ....155..212G}}</ref> This is consistent with previous studies, but the derived luminosity from different authors varies from {{solar luminosity|86,000}} to {{solar luminosity|186,000}}.<ref name=fok/><ref name=mauron/><ref name=verhoelst/> Older studies frequently calculated higher luminosities, lower temperatures, and consequently larger values for the radius.<ref name=dejager/>
The temperature has been calculated from the spectrum using a DUSTY model,<ref name=ivezic/> giving an effective photospheric temperature of 3,500 K and a temperature of 1,000 K for the surrounding dust torus.<ref name=michael>{{cite journal|doi=10.3847/1538-3881/aab961|title=Searching for Cool Dust. II. Infrared Imaging of the OH/IR Supergiants, NML Cyg, VX SGR, S Per, and the Normal Red Supergiants RS per and T per|year=2018|last1=Gordon|first1=Michael S.|last2=Humphreys|first2=Roberta M.|last3=Jones|first3=Terry J.|last4=Shenoy|first4=Dinesh|last5=Gehrz|first5=Robert D.|last6=Helton|first6=L. Andrew|last7=Marengo|first7=Massimo|last8=Hinz|first8=Philip M.|last9=Hoffmann|first9=William F.|s2cid=73650032|journal=The Astronomical Journal|volume=155|issue=5|page=212|arxiv=1708.00018|bibcode=2018AJ....155..212G |doi-access=free }}</ref> This is consistent with previous studies, but the derived luminosity from different authors varies from {{solar luminosity|86,000}} to {{solar luminosity|186,000}}.<ref name=fok/><ref name=mauron/><ref name=verhoelst/> Older studies frequently calculated higher luminosities, lower temperatures, and consequently larger values for the radius.<ref name=dejager/>


The mass of S Persei is also uncertain, but expected to be around {{solar mass|20}}.<ref name=yates/> Mass is being lost at 2.4 to {{solar mass|{{val|2.6|e=-5}}}} per year,<ref name=michael>{{cite journal|doi=10.3847/1538-3881/aab961|title=Searching for Cool Dust. II. Infrared Imaging of the OH/IR Supergiants, NML Cyg, VX SGR, S Per, and the Normal Red Supergiants RS per and T per|year=2018|last1=Gordon|first1=Michael S.|last2=Humphreys|first2=Roberta M.|last3=Jones|first3=Terry J.|last4=Shenoy|first4=Dinesh|last5=Gehrz|first5=Robert D.|last6=Helton|first6=L. Andrew|last7=Marengo|first7=Massimo|last8=Hinz|first8=Philip M.|last9=Hoffmann|first9=William F.|s2cid=73650032|journal=The Astronomical Journal|volume=155|issue=5|page=212|arxiv=1708.00018|bibcode=2018AJ....155..212G}}</ref> leading to an extensive and complex circumstellar environment of gas and dust.<ref name=fok/>
The mass of S Persei is also uncertain, but expected to be around {{solar mass|20}}.<ref name=yates/> Mass is being lost at 2.4 to {{solar mass|{{val|2.6|e=-5}}}} per year,<ref name=michael>{{cite journal|doi=10.3847/1538-3881/aab961|title=Searching for Cool Dust. II. Infrared Imaging of the OH/IR Supergiants, NML Cyg, VX SGR, S Per, and the Normal Red Supergiants RS per and T per|year=2018|last1=Gordon|first1=Michael S.|last2=Humphreys|first2=Roberta M.|last3=Jones|first3=Terry J.|last4=Shenoy|first4=Dinesh|last5=Gehrz|first5=Robert D.|last6=Helton|first6=L. Andrew|last7=Marengo|first7=Massimo|last8=Hinz|first8=Philip M.|last9=Hoffmann|first9=William F.|s2cid=73650032|journal=The Astronomical Journal|volume=155|issue=5|page=212|arxiv=1708.00018|bibcode=2018AJ....155..212G |doi-access=free }}</ref> leading to an extensive and complex circumstellar environment of gas and dust.<ref name=fok/>


==Location==
==Location==
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<ref name=dejager>{{cite journal|bibcode=1988A&AS...72..259D|title=Mass loss rates in the Hertzsprung-Russell diagram|journal=Astronomy and Astrophysics Supplement Series|volume=72|pages=259|last1=De Jager|first1=C.|last2=Nieuwenhuijzen|first2=H.|last3=Van Der Hucht|first3=K. A.|year=1988}}</ref>
<ref name=dejager>{{cite journal|bibcode=1988A&AS...72..259D|title=Mass loss rates in the Hertzsprung-Russell diagram|journal=Astronomy and Astrophysics Supplement Series|volume=72|pages=259|last1=De Jager|first1=C.|last2=Nieuwenhuijzen|first2=H.|last3=Van Der Hucht|first3=K. A.|year=1988}}</ref>


<ref name=ivezic>{{cite arxiv|eprint=astro-ph/9910475|title=User Manual for DUSTY|last1=Ivezic|first1=Zeljko|last2=Nenkova|first2=Maia|last3=Elitzur|first3=Moshe|year=1999}}</ref>
<ref name=ivezic>{{cite arXiv|eprint=astro-ph/9910475|title=User Manual for DUSTY|last1=Ivezic|first1=Zeljko|last2=Nenkova|first2=Maia|last3=Elitzur|first3=Moshe|year=1999}}</ref>


<ref name=thompson>{{cite journal|bibcode=2003AAS...203.4907T|title=Interferometric observations of the supergiant S Persei: Evidence for axial symmetry and the warm molecular layer|journal=American Astronomical Society Meeting 203|volume=203|pages=49.07|last1=Thompson|first1=R. R.|last2=Creech-Eakman|first2=M. J.|year=2003}}</ref>
<ref name=thompson>{{cite journal|bibcode=2003AAS...203.4907T|title=Interferometric observations of the supergiant S Persei: Evidence for axial symmetry and the warm molecular layer|journal=American Astronomical Society Meeting 203|volume=203|pages=49.07|last1=Thompson|first1=R. R.|last2=Creech-Eakman|first2=M. J.|year=2003}}</ref>
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<ref name=smith>{{cite journal|bibcode=1974JAVSO...3...20S|title=S Persei a Semi-Regular Variable with Two Periods|journal=Journal of the American Association of Variable Star Observers|volume=3|issue=1|pages=20|last1=Smith|first1=Horace A.|year=1974}}</ref>
<ref name=smith>{{cite journal|bibcode=1974JAVSO...3...20S|title=S Persei a Semi-Regular Variable with Two Periods|journal=Journal of the American Association of Variable Star Observers|volume=3|issue=1|pages=20|last1=Smith|first1=Horace A.|year=1974}}</ref>


<ref name=kiss>{{cite journal|bibcode=2006MNRAS.372.1721K|arxiv=astro-ph/0608438|title=Variability in red supergiant stars: Pulsations, long secondary periods and convection noise|journal=Monthly Notices of the Royal Astronomical Society|volume=372|issue=4|pages=1721–1734|last1=Kiss|first1=L. L.|last2=Szabó|first2=Gy. M.|last3=Bedding|first3=T. R.|s2cid=5203133|year=2006|doi=10.1111/j.1365-2966.2006.10973.x}}</ref>
<ref name=kiss>{{cite journal|bibcode=2006MNRAS.372.1721K|arxiv=astro-ph/0608438|title=Variability in red supergiant stars: Pulsations, long secondary periods and convection noise|journal=Monthly Notices of the Royal Astronomical Society|volume=372|issue=4|pages=1721–1734|last1=Kiss|first1=L. L.|last2=Szabó|first2=Gy. M.|last3=Bedding|first3=T. R.|s2cid=5203133|year=2006|doi=10.1111/j.1365-2966.2006.10973.x|doi-access=free }}</ref>

<ref name="aavso">{{cite web |title=Download Data |url=https://www.aavso.org/data-download |website=aavso.org |publisher=AAVSO |access-date=1 October 2021}}</ref>


<ref name=an>{{cite journal|doi=10.1002/asna.18740831005|title=Anzeige eines neuen veränderlichen Sternes (S Persei)|journal=Astronomische Nachrichten|volume=83|issue=10|pages=157–158|year=1874|last1=Krüger|first1=A.|bibcode=1874AN.....83..157K|url=https://zenodo.org/record/1424685}}</ref>
<ref name=an>{{cite journal|doi=10.1002/asna.18740831005|title=Anzeige eines neuen veränderlichen Sternes (S Persei)|journal=Astronomische Nachrichten|volume=83|issue=10|pages=157–158|year=1874|last1=Krüger|first1=A.|bibcode=1874AN.....83..157K|url=https://zenodo.org/record/1424685}}</ref>
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<ref name=asaki>{{cite journal|last1=Asaki|first1=Y.|last2=Deguchi|first2=S.|last3=Imai|first3=H.|last4=Hachisuka|first4=K.|last5=Miyoshi|first5=M.|last6=Honma|first6=M.|s2cid=119183897|title=Distance and Proper Motion Measurement of the Red Supergiant, S Persei, with Vlbi H2O Maser Astrometry|journal=The Astrophysical Journal|volume=721|issue=1|year=2010|pages=267–277|issn=0004-637X|doi=10.1088/0004-637X/721/1/267|bibcode=2010ApJ...721..267A|arxiv = 1007.4874 }}</ref>
<ref name=asaki>{{cite journal|last1=Asaki|first1=Y.|last2=Deguchi|first2=S.|last3=Imai|first3=H.|last4=Hachisuka|first4=K.|last5=Miyoshi|first5=M.|last6=Honma|first6=M.|s2cid=119183897|title=Distance and Proper Motion Measurement of the Red Supergiant, S Persei, with Vlbi H2O Maser Astrometry|journal=The Astrophysical Journal|volume=721|issue=1|year=2010|pages=267–277|issn=0004-637X|doi=10.1088/0004-637X/721/1/267|bibcode=2010ApJ...721..267A|arxiv = 1007.4874 }}</ref>


<ref name=yates>{{cite journal|bibcode=1994MNRAS.270..958Y|title=Circumstellar Envelope Structure of Late Type Stars as Revealed by MERLIN Observations of 22-GHZ Water Masers|journal=Monthly Notices of the Royal Astronomical Society|volume=270|issue=4|pages=958|last1=Yates|first1=J. A.|last2=Cohen|first2=R. J.|year=1994|doi=10.1093/mnras/270.4.958}}</ref>
<ref name=yates>{{cite journal|bibcode=1994MNRAS.270..958Y|title=Circumstellar Envelope Structure of Late Type Stars as Revealed by MERLIN Observations of 22-GHZ Water Masers|journal=Monthly Notices of the Royal Astronomical Society|volume=270|issue=4|pages=958|last1=Yates|first1=J. A.|last2=Cohen|first2=R. J.|year=1994|doi=10.1093/mnras/270.4.958|doi-access=free}}</ref>


<ref name=mauron>{{cite journal|bibcode=2011A&A...526A.156M|arxiv=1010.5369|title=The mass-loss rates of red supergiants and the de Jager prescription|journal=Astronomy and Astrophysics|volume=526|pages=A156|last1=Mauron|first1=N.|last2=Josselin|first2=E.|s2cid=119276502|year=2011|doi=10.1051/0004-6361/201013993}}</ref>
<ref name=mauron>{{cite journal|bibcode=2011A&A...526A.156M|arxiv=1010.5369|title=The mass-loss rates of red supergiants and the de Jager prescription|journal=Astronomy and Astrophysics|volume=526|pages=A156|last1=Mauron|first1=N.|last2=Josselin|first2=E.|s2cid=119276502|year=2011|doi=10.1051/0004-6361/201013993}}</ref>
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{{Stars of Perseus}}
{{Stars of Perseus}}


{{DEFAULTSORT:S Persei}}
[[Category:M-type supergiants]]
[[Category:M-type supergiants]]
[[Category:Perseus (constellation)]]
[[Category:Perseus (constellation)]]

Latest revision as of 13:23, 29 August 2024

S Persei
Location of S Persei (circled) near the Double Cluster (north is left)
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 2h 22m 51.70928s[1]
Declination 58° 31′ 11.4476″[1]
Apparent magnitude (V) +9.23[2] (7.9 - 12.0[3])
Characteristics
Spectral type M3 Iae–M7[3]
B−V color index +2.65[2]
Variable type SRc[3]
Astrometry
Radial velocity (Rv)-39.71[4] km/s
Proper motion (μ) RA: –0.49 ± 0.23[5] mas/yr
Dec.: −1.19 ± 0.20[5] mas/yr
Parallax (π)0.413 ± 0.017 mas[5]
Distance7,900 ± 300 ly
(2,420 ± 100 pc)
Absolute magnitude (MV)–6.36 (at mV 9.23)[2]
Details
Mass20[6] M☉
Radius1,298+64
−57[7] – 1,364±6[8] R☉
Luminosity123,000[9] – 186,000[10] L☉
Surface gravity (log g)0.0[11] cgs
Temperature3,000[12] – 3,600[10] K
Other designations
S Per, HD 14528, HIP 11093, BD+57°552, SAO 23261, WDS J02229+5835, AAVSO 0215+58
Database references
SIMBADdata

S Persei is a red supergiant or hypergiant located near the Double Cluster in Perseus, north of the cluster NGC 869. It is a member of the Perseus OB1 association and one of the largest known stars. If placed in the Solar System, its photosphere would engulf the orbit of Jupiter. It is also a semiregular variable, a star whose variations are less regular than those of Mira variables.

Discovery

[edit]

S Persei was named by German astronomer Adalbert Krueger in 1874 after observing that it varied in brightness.[13] It was subsequently listed in major stellar catalogues of that era as HD 14528 and BD+57°552.

Variability

[edit]
A visual band light curve for S Persei, plotted from AAVSO data[14]

S Persei varies slowly by several magnitudes, a factor of over 40 in brightness. It has a main period of somewhat over two years, but shows significant unpredictability. There is a strong variation in the amplitude from around one magnitude to about four magnitudes, and these have been interpreted as beats due to a second period of about 940 days.[15] Other analyses find only the primary period of 813 ± 60 days.[16]

S Persei is classified as a semiregular variable star of type SRc, indicating that it is a supergiant, and it has one of the largest visual amplitudes of any variable of this type.[3] While the General Catalogue of Variable Stars lists it as varying between magnitudes 7.9 and 12.0, it has since been seen fainter.[16]

The spectral type of S Persei also varies. Typically it is a red supergiant of spectral class M3 or M4, but particularly at deep visual minima it may show a much cooler spectral type of M7 or M8, highly unusual for a supergiant.[17]

Properties

[edit]

Many of the visually bright variable stars belong to this class of semiregulars, as these stars are extremely large and luminous, and hence visible across long distances. S Persei has been described as a hypergiant[18] and has a radius over 700 times the sun's radius (R☉).[2] Its angular diameter has been measured directly and found to be somewhat elliptical. Modelled as a uniform disk, the radius corresponds to 1,212 ± 124 R☉.[19]

The temperature has been calculated from the spectrum using a DUSTY model,[20] giving an effective photospheric temperature of 3,500 K and a temperature of 1,000 K for the surrounding dust torus.[21] This is consistent with previous studies, but the derived luminosity from different authors varies from 86,000 L☉ to 186,000 L☉.[10][22][23] Older studies frequently calculated higher luminosities, lower temperatures, and consequently larger values for the radius.[24]

The mass of S Persei is also uncertain, but expected to be around 20 M☉.[6] Mass is being lost at 2.4 to 2.6×10−5 M☉ per year,[21] leading to an extensive and complex circumstellar environment of gas and dust.[10]

Location

[edit]

S Persei is surrounded by clouds containing water molecules which produce maser emission. This allows the distance to be measured very accurately using very long baseline interferometry, giving an annual parallax of 0.413 ± 0.017 milliarcseconds. For comparison the Gaia Data Release 2 parallax is 0.2217±0.1214 mas.[25] It lies somewhat further away than the centres of the Double Cluster open clusters, but definitely within the Per OB1 association and the Perseus Arm of the galaxy.[5]

S Persei is a double star. The red supergiant has an A0 11th magnitude companion at 69".[26] There are also several other 8th to 10th magnitude stars within half a degree of S Persei.[27]

References

[edit]
  1. ^ a b Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  2. ^ a b c d Emily M. Levesque; Philip Massey; K. A. G. Olsen; Bertrand Plez; et al. (August 2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. S2CID 15109583.
  3. ^ a b c d Samus', N. N.; Goranskii, V. P.; Durlevich, O. V.; Zharova, A. V.; Kazarovets, E. V.; Kireeva, N. N.; Pastukhova, E. N.; Williams, D. B.; Hazen, M. L. (2003). "An Electronic Version of the Second Volume of the General Catalogue of Variable Stars with Improved Coordinates". Astronomy Letters. 29 (7): 468. Bibcode:2003AstL...29..468S. doi:10.1134/1.1589864. S2CID 16299532.
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