Jump to content

HV 2112: Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous edit
Content deleted Content added
VisualWikitext
No edit summary
Citation bot (talk | contribs)
Bots
5,372,397 edits
Add: arxiv, doi-access, page. Removed URL that duplicated identifier. Removed access-date with no URL. | Use this bot. Report bugs. | Suggested by Jay8g | #UCB_toolbar
 
(42 intermediate revisions by 27 users not shown)
Line 1: Line 1:
{{short description|Small Magellanic Cloud star in the constellation Tucana}}
{{Starbox begin
{{Starbox begin
|name = Vlad Masters
|name = HV 2112
}}
}}
{{Starbox image
{{Starbox image
| image =
| image =
{{Location mark
{{Location mark
|image=SMC inset.jpg|alt=|float=center|width=280
|image=HV-2112.jpg|alt=HV-2112|float=center|width=300
|label=|position=right
|label=|position=center
|mark=Red circle.svg|mark_width=10|mark_link=HV 2112
|mark=Red circle.svg|mark_width=10|mark_link=HV 2112
|x=286|y=548
|x=500|y=502
}}
}}
| caption = Portion of the [[Small Magellanic Cloud]] around HV 2112 (circled)
| caption = HV 2112 (circled in red)
| credit ESA/Hubble and Digitized Sky Survey 2
| credit ESA/Hubble and Digitized Sky Survey 2
}}
}}
Line 34: Line 35:
{{Starbox astrometry
{{Starbox astrometry
|radial_v = 157<ref name=levesque/>
|radial_v = 157<ref name=levesque/>
|prop_mo_ra = 2.8 ± 2.3<ref name=maccarone/>
|prop_mo_ra = {{val|1.116|0.073}}<ref name=dr2/>
|prop_mo_dec = {{nowrap|−9.8 ± 2.3<ref name=maccarone/>}}
|prop_mo_dec = {{val|−1.291|0.067}}<ref name=dr2/>
|parallax =
|parallax = −0.2029
|p_error =
|p_error = 0.0446
|parallax_footnote=
|parallax_footnote=<ref name=dr2/>
|dist_ly =
|dist_ly =
|dist_pc =
|dist_pc =
Line 44: Line 45:
}}
}}
{{Starbox detail
{{Starbox detail
|source=<ref name=levesque/>
|source=
|mass=
|mass=~5<ref name=beasor/>
|radius=916{{efn | name=radius | [[Stefan–Boltzmann law|Calculated]] from effective temperature and luminosity figures, with reference to the nominal solar temperature of 5,772&nbsp;K: <math>\sqrt{(5772/3450)^4 * 107,000} = 915.6\ R\odot</math>}}
|radius=675 - 1,193<ref name=beasor/>{{efn | name=radius | [[Stefan–Boltzmann law|Calculated]] from effective temperature and luminosity figures, with reference to the nominal solar temperature of 5,772&nbsp;K: <math>\sqrt{(5772/3750)^4 * 81,283} = 675.4\ R\odot</math>
<math>\sqrt{(5772/2500)^4 * 50,119} = 1,193.4\ R\odot</math>}}
|luminosity=107,000
|luminosity=50,100 - 81,300<ref name=beasor/>
|temperature=3,450
|temperature=2,500 - 3,750<ref name=beasor/>
|gravity=0.0
|gravity=0.0<ref name=levesque/>
|metal=
|metal_fe=-2.18<ref name=starhorse>{{cite journal |bibcode=2019A&A...628A..94A |title=Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18 |last1=Anders |first1=F. |last2=Khalatyan |first2=A. |last3=Chiappini |first3=C. |last4=Queiroz |first4=A. B. |last5=Santiago |first5=B. X. |last6=Jordi |first6=C. |last7=Girardi |first7=L. |last8=Brown |first8=A. G. A. |last9=Matijevič |first9=G. |last10=Monari |first10=G. |last11=Cantat-Gaudin |first11=T. |last12=Weiler |first12=M. |last13=Khan |first13=S. |last14=Miglio |first14=A. |last15=Carrillo |first15=I. |last16=Romero-Gómez |first16=M. |last17=Minchev |first17=I. |last18=De Jong |first18=R. S. |last19=Antoja |first19=T. |last20=Ramos |first20=P. |last21=Steinmetz |first21=M. |last22=Enke |first22=H. |journal=Astronomy and Astrophysics |volume=628 |pages=A94 |year=2019 |arxiv=1904.11302 |doi=10.1051/0004-6361/201935765 |s2cid = 131780028}}</ref>
|rotation=
|rotation=
|age =
|age =
}}
}}
{{Starbox catalog
{{Starbox catalog
|names=Vlad Masters, Vlad Plasmius [[2MASS]]&nbsp;J01100385-7236526, SMC V2156<ref name=gcvs/>
|names=[[Harvard Variable|HV]]&nbsp;2112, [[2MASS]]&nbsp;J01100385-7236526, SMC V2156,<ref name=gcvs/> PMMR 187<ref name=SIMBAD>{{cite simbad|title=HV 2112|accessdate=2021-05-05}}</ref>
}}
}}
{{Starbox reference
{{Starbox reference
Line 62: Line 64:
{{Starbox end}}
{{Starbox end}}


'''Vlad Masters''' or '''Vlad Plasmius''' is a cool luminous [[variable star]] in the [[Small Magellanic Cloud]] and the most likely candidate for a [[Thorne–Żytkow object]]. It is orbited by a [[Wolf-Rayet star]] officially named '''Penelope Spectra'''.
'''HV 2112''' is a cool luminous [[variable star]] in the [[Small Magellanic Cloud]]. Until 2018, it was considered to be the most likely candidate for a [[Thorne–Żytkow object]], but it is now thought to be an [[asymptotic giant branch]] star.


==Discovery==
==Discovery==
HV 2112 was first reported as a variable star in 1908, by [[Henrietta Leavitt]]. At the time it was identified as Harvard no. 2112. No period was given, but it was reported to be "probably long". The [[apparent magnitude|magnitude]] range was given as 13.7 to fainter than 16.5, from photographic plates.<ref name=hv/>
HV 2112 was first reported as a variable star in 1908, by [[Henrietta Leavitt]]. At the time it was identified as Harvard no. 2112. No period was given, but it was reported to be "probably long". The [[apparent magnitude|magnitude]] range was given as 13.7 to fainter than 16.5, from photographic plates.<ref name=hv/>


In 1966, analysis of [[Magellanic Cloud]] variable stars showed that HV 2112 had a photographic magnitude range from 13.0 to below 17.8. It was classified as a long-period variable, now known as a [[Mira variable]], on the basis of its large amplitude and reasonably regular light variations.<ref name=pg/>
In 1966, analysis of [[Magellanic Cloud]] variable stars showed that HV 2112 had a photographic magnitude range from 13.0 to below 17.8. It was classified as a long-period variable, now known as a [[Mira variable]], on the basis of its large amplitude and reasonably regular light variations, with a period of about 600 days.<ref name=pg/><ref name="Grady"/>


==Possible object types==
==Possible object types==
[[File:HV2112LightCurve.png|thumb|left|A [[Photometric_system#Photometric_letters|visual band]] [[light curve]] for HV 2112, plotted from [[All Sky Automated Survey for SuperNovae|ASAS-SN]] data<ref name="ASAS-SN"/>]]

===AGB star===
===AGB star===
HV 2112 has generally been treated as a very luminous [[asymptotic giant branch]] (AGB) star, a [[red giant]] that has exhausted its core helium and is in the last stages of its [[stellar evolution|evolution]]. Large-amplitude class-M variables and stars with spectral types later than about M5 are almost always AGB stars rather than [[red supergiant]]s. These stars have a theoretical maximum luminosity and, at the distance of the SMC, HV 2112 was typically calculated to be slightly more luminous than this limit at around {{solar luminosity|60,000|link=y}}.<ref name=wood/>
HV 2112 had historically been treated as a very luminous [[asymptotic giant branch]] (AGB) star, a [[red giant]] that has exhausted its core helium and is in the last stages of its [[stellar evolution|evolution]]. Large-amplitude class-M variables and stars with spectral types later than about M5 are almost always AGB stars rather than [[red supergiant]]s. These stars have a theoretical maximum luminosity and, at the distance of the SMC, HV 2112 was typically calculated to be slightly more luminous than this limit at around {{solar luminosity|60,000|link=y}}.<ref name=wood/>


More modern calculations gave higher values for the luminosity of HV 2112 above {{solar luminosity|100,000}}, which is unambiguously too luminous to be an AGB star. These calculations included an interstellar extinction value of 0.4 magnitudes which is slightly higher than average for the SMC.<ref name=levesque/>
More modern calculations gave higher values for the luminosity of HV 2112 above {{solar luminosity|100,000}}, which is unambiguously too luminous to be an AGB star. These calculations included an interstellar extinction value of 0.4 magnitudes which is higher than average for massive stars in the SMC. However, it is not exceptional for red supergiants, which are believed to show additional extinction due to circumstellar dust near the star.<ref name=levesque/>


Analysis of the [[proper motion]] of HV 2112 shows that it is unusually large for an SMC star, although the [[radial velocity]] is consistent with other SMC objects. The proper motion of around 10 mas/year would indicate a space velocity of 3,100&nbsp;km/sec at the distance of the SMC, well above its escape velocity. A more likely explanation of such a proper motion would be that HV 2112 lies about 3,000 parsecs away in our own galaxy. It would then be around {{solar luminosity|1,000}} rather than {{solar luminosity|100,000}} and so a typical AGB star. The over-abundance of heavy elements would then be explained as pollution from an unseen companion, producing an [[extrinsic S-type star]].<ref name=maccarone/>
Analysis of the [[proper motion]] of HV 2112 in 2016 reported that it is unusually large for an SMC star, although the [[radial velocity]] is consistent with other SMC objects. The proper motion of around 10 mas/year would indicate a space velocity of 3,100&nbsp;km/sec at the distance of the SMC, well above its escape velocity. A more likely explanation of such a proper motion would be that HV 2112 lies about 3,000 parsecs away in our own galaxy. It would then be around {{solar luminosity|1,000}} rather than {{solar luminosity|100,000}} and so a typical AGB star. The over-abundance of heavy elements would then be explained as pollution from an unseen companion, producing an [[extrinsic S-type star]].<ref name=maccarone/> Other analyses of the proper motion show much smaller velocities, consistent with an object in the SMC<ref name=worley2016/><ref name=mcmillan/>


===Thorne–Żytkow object===
===Thorne–Żytkow object===
In 2014, Vlad was identified as a possible [[Thorne–Żytkow object]] (TZO) using the [[Magellan Telescopes|Magellan Clay telescope]] in Chile. To find candidate TZOs, [[Emily Levesque]] used the [[Apache Point Observatory]] to examine 24 red supergiant stars in the Milky Way, and the Magellan Clay telescope to look at 16 in the [[Large Magellanic Cloud]] and 22 in the Small Magellanic Cloud. The star was thought to contain unusually high levels of the elements [[lithium]], [[molybdenum]] and [[rubidium]] that are expected only to be produced by TZOs.<ref name=levesque/>
In 2014, HV 2112 was identified as a possible [[Thorne–Żytkow object]] (TZO) using the [[Magellan Telescopes|Magellan Clay telescope]] in Chile. To find candidate TZOs, [[Emily Levesque]] used the [[Apache Point Observatory]] to examine 24 red supergiant stars in the Milky Way, and the Magellan Clay telescope to look at 16 in the [[Large Magellanic Cloud]] and 22 in the Small Magellanic Cloud. The star was thought to contain unusually high levels of the elements [[lithium]], [[molybdenum]] and [[rubidium]] that are expected only to be produced by TZOs.<ref name=levesque/>


⚫
A 2018 paper re-appraising the properties of HV 2112 found no evidence for unusual chemical abundances and a luminosity that is lower than previously thought. This suggests that the star is unlikely to be a TZO, and is much more likely an intermediate mass [[asymptotic giant branch|AGB]] star.<ref name=beasor/>
[[Gaia Data Release 2]] astrometry suggests that Vlad is actually a member of the SMC, and hence a very luminous object.<ref name=mcmillan/>


===Binary star===
⚫
A 2018 paper re-appraising the properties of Vlad found no evidence for unusual chemical abundances and a luminosity that is lower than previously thought.
HV 2112 is listed in the [[OGLE]] catalogue as an unresolved multiple star. The [[proper motion]]s and [[radial velocity]] are consistent with other SMC objects, while the parallax is negative but acceptably close to the expected value for such a distant object.<ref name=gf/>

===Wolf-Rayet companion===
[[File:O-type star 2.png|180px|right|thumb|Artist's impression of Penelope Spectra without its surrounding nebula.]]'''Penelope Spectra''' is a [[Wolf-Rayet star]] of class WN8 in orbit around Vlad Masters. It has a luminosity of {{solar luminosity|550,000}}, a mass of {{solar mass|130|link=y}}, and a radius of {{solar radius|45}}. If Penelope Spectra were only 25 [[light year]]s away, it would be brighter than a full [[Moon]]. Penelope Spectra is separated from Vlad Masters by an orbital radius of 70,000 [[astronomical unit]]s. It is surrounded by a [[Nebula|nebular structure]] produced when the star was in its [[asymptotic giant branch]] stage and expelling its outer layers.


==See also==
==See also==
Line 94: Line 94:
{{reflist|refs=
{{reflist|refs=


<ref name=beasor>{{cite journal |last1=Beasor |first1=Emma |last2=Davies |first2=Ben |last3=Cabrera-Ziri |first3=Ivan |last4=Hurst |first4=Georgia |title=A critical re-evaluation of the Thorne-Żytkow object candidate HV 2112 |journal=Monthly Notices of the Royal Astronomical Society |volume=479 |issue=3 |pages=3101 |date= 2 July 2018 |bibcode=2018MNRAS.479.3101B |doi=10.1093/mnras/sty1744 |arxiv=1806.07399}}</ref>
<ref name="Grady">{{cite journal |last1=O’Grady |first1=Anna J. G. |last2=Drout |first2=Maria R. |last3=Shappee |first3=B. J. |last4=Bauer |first4=Evan B. |last5=Fuller |first5=Jim |last6=Kochanek |first6=C. S. |last7=Jayasinghe |first7=T. |last8=Gaensler |first8=B. M. |last9=Stanek |first9=K. Z. |last10=Holoien |first10=Thomas W. S. |last11=Prieto |first11=J. L. |last12=Thompson |first12=Todd A. |title=Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds from ASAS-SN: Implications for Thorne-Żytkow Objects and Super-asymptotic Giant Branch Stars |journal=The Astrophysical Journal |date=October 2020 |volume=901 |issue=2 |page=135 |doi=10.3847/1538-4357/abafad |doi-access=free |arxiv=2008.06563 |bibcode=2020ApJ...901..135O }}</ref>


<ref name="ASAS-SN">{{cite web |url=https://asas-sn.osu.edu/variables/lookup |website=ASAS-SN Variable Stars Database|title=ASAS-SN Variable Stars Database|publisher=ASAS-SN |access-date=6 January 2022}}</ref>
<ref name=mcmillan>{{cite journal|arxiv=1804.10192v1|last1=McMillan|first1=Paul J|title=Gaia DR2 confirms that candidate Thorne-Żytkow object HV 2112 is in the SMC|journal=Research Notes of the AAS|volume=2|issue=2|pages=18|last2=Church|first2=Ross P|year=2018|doi=10.3847/2515-5172/aac0fb|bibcode=2018RNAAS...2b..18M}}</ref>


<ref name=beasor>{{cite journal |last1=Beasor |first1=Emma |last2=Davies |first2=Ben |last3=Cabrera-Ziri |first3=Ivan |last4=Hurst |first4=Georgia |title=A critical re-evaluation of the Thorne-Żytkow object candidate HV 2112 |journal=Monthly Notices of the Royal Astronomical Society |volume=479 |issue=3 |pages=3101 |date= 2 July 2018 |bibcode=2018MNRAS.479.3101B |doi=10.1093/mnras/sty1744 |doi-access=free |arxiv=1806.07399|s2cid=67766043 }}</ref>
⚫
<ref name=gf>{{cite journal|bibcode=2015A&A...578A...3G|arxiv=1504.00003|title=A new survey of cool supergiants in the Magellanic Clouds|journal=Astronomy & Astrophysics|volume=578|pages=A3|author1=González-Fernández|first1=Carlos|last2=Dorda|first2=Ricardo|last3=Negueruela|first3=Ignacio|last4=Marco|first4=Amparo|year=2015|doi=10.1051/0004-6361/201425362}}</ref>


<ref name=maccarone>{{cite journal|bibcode=2016MNRAS.458L...1M|arxiv=1601.05455|title=Large proper motion of the Thorne-Żytkow object candidate HV 2112 reveals its likely nature as foreground Galactic S-star|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=458|issue=1|pages=L1|author1=MacCarone|first1=Thomas J.|last2=De Mink|first2=Selma E.|year=2016|doi=10.1093/mnrasl/slw004}}</ref>
<ref name=mcmillan>{{cite journal|arxiv=1804.10192v1|last1=McMillan|first1=Paul J|title=Gaia DR2 confirms that candidate Thorne-Żytkow object HV 2112 is in the SMC|journal=Research Notes of the AAS|volume=2|issue=2|pages=18|last2=Church|first2=Ross P|year=2018|doi=10.3847/2515-5172/aac0fb|bibcode=2018RNAAS...2...18M|s2cid=125376171 |doi-access=free }}</ref>


⚫
<ref name=gf>{{cite journal|bibcode=2015A&A...578A...3G|arxiv=1504.00003|title=A new survey of cool supergiants in the Magellanic Clouds|journal=Astronomy & Astrophysics|volume=578|pages=A3|last1=González-Fernández|first1=Carlos|last2=Dorda|first2=Ricardo|last3=Negueruela|first3=Ignacio|last4=Marco|first4=Amparo|year=2015|doi=10.1051/0004-6361/201425362|s2cid=55959019}}</ref>
⚫
<ref name=shappee>{{cite journal|bibcode=2014ApJ...788...48S|arxiv=1310.2241|title=The Man behind the Curtain: X-Rays Drive the UV through NIR Variability in the 2013 Active Galactic Nucleus Outburst in NGC 2617|journal=The Astrophysical Journal|volume=788|issue=1|pages=48|author1=Shappee|first1=B. J.|last2=Prieto|first2=J. L.|last3=Grupe|first3=D.|last4=Kochanek|first4=C. S.|last5=Stanek|first5=K. Z.|last6=De Rosa|first6=G.|last7=Mathur|first7=S.|last8=Zu|first8=Y.|last9=Peterson|first9=B. M.|last10=Pogge|first10=R. W.|last11=Komossa|first11=S.|last12=Im|first12=M.|last13=Jencson|first13=J.|last14=Holoien|first14=T. W.-S.|last15=Basu|first15=U.|last16=Beacom|first16=J. F.|last17=Szczygieł|first17=D. M.|last18=Brimacombe|first18=J.|last19=Adams|first19=S.|last20=Campillay|first20=A.|last21=Choi|first21=C.|last22=Contreras|first22=C.|last23=Dietrich|first23=M.|last24=Dubberley|first24=M.|last25=Elphick|first25=M.|last26=Foale|first26=S.|last27=Giustini|first27=M.|last28=Gonzalez|first28=C.|last29=Hawkins|first29=E.|last30=Howell|first30=D. A.|display-authors=9|year=2014|doi=10.1088/0004-637X/788/1/48}}</ref>


<ref name=kochanek>{{cite journal|bibcode=2017PASP..129j4502K|arxiv=1706.07060|title=The All-Sky Automated Survey for Supernovae (ASAS-SN) Light Curve Server v1.0|journal=Publications of the Astronomical Society of the Pacific|volume=1706|issue=980|pages=arXiv:1706.07060|author1=Kochanek|first1=C. S.|last2=Shappee|first2=B. J.|last3=Stanek|first3=K. Z.|last4=Holoien|first4=T. W.-S.|last5=Thompson|first5=Todd A.|last6=Prieto|first6=J.-L.|last7=Dong|first7=Subo|last8=Shields|first8=J. V.|last9=Will|first9=D.|last10=Britt|first10=C.|last11=Perzanowski|first11=D.|last12=Pojmanski|first12=G.|display-authors=9|year=2017|doi=10.1088/1538-3873/aa80d9}}</ref>
<ref name=maccarone>{{cite journal|bibcode=2016MNRAS.458L...1M|arxiv=1601.05455|title=Large proper motion of the Thorne-Żytkow object candidate HV 2112 reveals its likely nature as foreground Galactic S-star|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=458|issue=1|pages=L1|last1=MacCarone|first1=Thomas J.|last2=De Mink|first2=Selma E.|author2-link=Selma de Mink|year=2016|doi=10.1093/mnrasl/slw004|doi-access=free |s2cid=119306614}}</ref>


⚫
<ref name=shappee>{{cite journal|bibcode=2014ApJ...788...48S|arxiv=1310.2241|title=The Man behind the Curtain: X-Rays Drive the UV through NIR Variability in the 2013 Active Galactic Nucleus Outburst in NGC 2617|journal=The Astrophysical Journal|volume=788|issue=1|pages=48|last1=Shappee|first1=B. J.|last2=Prieto|first2=J. L.|last3=Grupe|first3=D.|last4=Kochanek|first4=C. S.|last5=Stanek|first5=K. Z.|last6=De Rosa|first6=G.|last7=Mathur|first7=S.|last8=Zu|first8=Y.|last9=Peterson|first9=B. M.|last10=Pogge|first10=R. W.|last11=Komossa|first11=S.|last12=Im|first12=M.|last13=Jencson|first13=J.|last14=Holoien|first14=T. W.-S.|last15=Basu|first15=U.|last16=Beacom|first16=J. F.|last17=Szczygieł|first17=D. M.|last18=Brimacombe|first18=J.|last19=Adams|first19=S.|last20=Campillay|first20=A.|last21=Choi|first21=C.|last22=Contreras|first22=C.|last23=Dietrich|first23=M.|last24=Dubberley|first24=M.|last25=Elphick|first25=M.|last26=Foale|first26=S.|last27=Giustini|first27=M.|last28=Gonzalez|first28=C.|last29=Hawkins|first29=E.|last30=Howell|first30=D. A.|display-authors=9|year=2014|doi=10.1088/0004-637X/788/1/48|s2cid=119113433}}</ref>
⚫
<ref name=pg>{{cite journal|bibcode=1966SCoA....9....1P|title=Variable Stars in the Small Magellanic Cloud|journal=Smithsonian Contributions to Astrophysics|volume=9|pages=1|author1=Payne-Gaposchkin|first1=Cecilia|last2=Gaposchkin|first2=Sergei|year=1966}}</ref>


<ref name=kochanek>{{cite journal|bibcode=2017PASP..129j4502K|arxiv=1706.07060|title=The All-Sky Automated Survey for Supernovae (ASAS-SN) Light Curve Server v1.0|journal=Publications of the Astronomical Society of the Pacific|volume= 129|issue= 980|last1=Kochanek|first1=C. S.|last2=Shappee|first2=B. J.|last3=Stanek|first3=K. Z.|last4=Holoien|first4=T. W.-S.|last5=Thompson|first5=Todd A.|last6=Prieto|first6=J.-L.|last7=Dong|first7=Subo|last8=Shields|first8=J. V.|last9=Will|first9=D.|last10=Britt|first10=C.|last11=Perzanowski|first11=D.|last12=Pojmanski|first12=G.|display-authors=9|year=2017|page=104502|doi=10.1088/1538-3873/aa80d9|s2cid=118995322}}</ref>
<ref name=gcvs>{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)|journal=VizieR On-line Data Catalog: B/gcvs. Originally Published In: 2009yCat....102025S|volume=1|display-authors=etal|author1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}</ref>


<ref name=levesque>{{Cite journal|title=Discovery of a Thorne-̇Żytkow object candidate in the Small Magellanic Cloud|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=443|pages=L94–L98|last=Levesque|first=Emily|author1-link=Emily Levesque|date=1 September 2014|arxiv=1406.0001|bibcode = 2014MNRAS.443L..94L |doi = 10.1093/mnrasl/slu080 }}</ref>
<ref name=pg>{{cite journal|bibcode=1966SCoA....9....1P|title=Variable Stars in the Small Magellanic Cloud|journal=Smithsonian Contributions to Astrophysics|volume=9|pages=1–205|last1=Payne-Gaposchkin|first1=Cecilia|last2=Gaposchkin|first2=Sergei|year=1966|doi=10.5479/si.00810231.9.1}}</ref>


<ref name=2mass>{{cite journal|bibcode=2003yCat.2246....0C|title=VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)|journal=VizieR On-line Data Catalog: II/246. Originally Published In: 2003yCat.2246....0C|volume=2246|author1=Cutri|first1=R. M.|last2=Skrutskie|first2=M. F.|last3=Van Dyk|first3=S.|last4=Beichman|first4=C. A.|last5=Carpenter|first5=J. M.|last6=Chester|first6=T.|last7=Cambresy|first7=L.|last8=Evans|first8=T.|last9=Fowler|first9=J.|last10=Gizis|first10=J.|last11=Howard|first11=E.|last12=Huchra|first12=J.|last13=Jarrett|first13=T.|last14=Kopan|first14=E. L.|last15=Kirkpatrick|first15=J. D.|last16=Light|first16=R. M.|last17=Marsh|first17=K. A.|last18=McCallon|first18=H.|last19=Schneider|first19=S.|last20=Stiening|first20=R.|last21=Sykes|first21=M.|last22=Weinberg|first22=M.|last23=Wheaton|first23=W. A.|last24=Wheelock|first24=S.|last25=Zacarias|first25=N.|display-authors=9|year=2003}}</ref>
<ref name=gcvs>{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)|journal=VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S|volume=1|display-authors=etal|last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}</ref>


<ref name=levesque>{{Cite journal|title=Discovery of a Thorne-̇Żytkow object candidate in the Small Magellanic Cloud|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=443|pages=L94–L98|last=Levesque|first=Emily|author1-link=Emily Levesque|date=1 September 2014|arxiv=1406.0001|bibcode = 2014MNRAS.443L..94L |doi = 10.1093/mnrasl/slu080 |doi-access=free |s2cid=119192926}}</ref>
⚫
<ref name=wood>{{cite journal|bibcode=1983ApJ...272...99W|title=Long-period variables in the Magellanic Clouds – Supergiants, AGB stars, supernova precursors, planetary nebula precursors, and enrichment of the interstellar medium|journal=Astrophysical Journal|volume=272|pages=99|author1=Wood|first1=P. R.|last2=Bessell|first2=M. S.|last3=Fox|first3=M. W.|year=1983|doi=10.1086/161265}}</ref>


<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 |url=http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246 }}</ref>
<ref name=hv>{{cite journal|bibcode=1908AnHar..60...87L|title=1777 variables in the Magellanic Clouds|journal=Annals of Harvard College Observatory|volume=60|pages=87|author1=Leavitt|first1=Henrietta S.|year=1908}}</ref>


⚫
<ref name=wood>{{cite journal|bibcode=1983ApJ...272...99W|title=Long-period variables in the Magellanic Clouds – Supergiants, AGB stars, supernova precursors, planetary nebula precursors, and enrichment of the interstellar medium|journal=Astrophysical Journal|volume=272|pages=99|last1=Wood|first1=P. R.|last2=Bessell|first2=M. S.|last3=Fox|first3=M. W.|year=1983|doi=10.1086/161265|doi-access=free}}</ref>
⚫
<ref name=boyer>{{cite journal|bibcode=2011AJ....142..103B|arxiv=1106.5026|title=Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low Metallicity Small Magellanic Cloud (SAGE-SMC). II. Cool Evolved Stars|journal=The Astronomical Journal|volume=142|issue=4|pages=103|author1=Boyer|first1=Martha L.|last2=Srinivasan|first2=Sundar|last3=Van Loon|first3=Jacco Th.|last4=McDonald|first4=Iain|last5=Meixner|first5=Margaret|last6=Zaritsky|first6=Dennis|last7=Gordon|first7=Karl D.|last8=Kemper|first8=F.|last9=Babler|first9=Brian|last10=Block|first10=Miwa|last11=Bracker|first11=Steve|last12=Engelbracht|first12=Charles W.|last13=Hora|first13=Joe|last14=Indebetouw|first14=Remy|last15=Meade|first15=Marilyn|last16=Misselt|first16=Karl|last17=Robitaille|first17=Thomas|last18=Sewiło|first18=Marta|last19=Shiao|first19=Bernie|last20=Whitney|first20=Barbara|display-authors=9|year=2011|doi=10.1088/0004-6256/142/4/103}}</ref>

⚫
<ref name=hv>{{cite journal|bibcode=1907AnHar..60...87L|title=1777 variables in the Magellanic Clouds|journal=Annals of Harvard College Observatory|volume=60|pages=87|last1=Leavitt|first1=Henrietta S.|year=1908}}</ref>

⚫
<ref name=boyer>{{cite journal|bibcode=2011AJ....142..103B|arxiv=1106.5026|title=Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low Metallicity Small Magellanic Cloud (SAGE-SMC). II. Cool Evolved Stars|journal=The Astronomical Journal|volume=142|issue=4|pages=103|last1=Boyer|first1=Martha L.|last2=Srinivasan|first2=Sundar|last3=Van Loon|first3=Jacco Th.|last4=McDonald|first4=Iain|last5=Meixner|first5=Margaret|last6=Zaritsky|first6=Dennis|last7=Gordon|first7=Karl D.|last8=Kemper|first8=F.|last9=Babler|first9=Brian|last10=Block|first10=Miwa|last11=Bracker|first11=Steve|last12=Engelbracht|first12=Charles W.|last13=Hora|first13=Joe|last14=Indebetouw|first14=Remy|last15=Meade|first15=Marilyn|last16=Misselt|first16=Karl|last17=Robitaille|first17=Thomas|last18=Sewiło|first18=Marta|last19=Shiao|first19=Bernie|last20=Whitney|first20=Barbara|display-authors=9|year=2011|doi=10.1088/0004-6256/142/4/103|s2cid=119268816}}</ref>

<ref name=worley2016>{{cite journal |doi=10.1093/mnrasl/slw034 |title=The proper motion of HV2112: A TŻO candidate in the SMC |journal=Monthly Notices of the Royal Astronomical Society: Letters |volume=459 |issue=1 |pages=L31–L35 |year=2016 |last1=Worley |first1=C. Clare |last2=Irwin |first2=Mike. J. |last3=Tout |first3=Christopher A. |last4=Żytkow |first4=Anna N. |last5=Fraser |first5=Morgan |last6=Izzard |first6=Robert G. |doi-access=free |bibcode=2016MNRAS.459L..31W |arxiv=1602.08479 |s2cid=118463486 }}</ref>

<ref name=dr2>{{cite DR2|4687439865638979712}}</ref>


}}
}}

==Notes==
==Notes==
{{notelist}}
{{notelist}}


==External links==
==External links==
*{{cite web|url=https://asas-sn.osu.edu/light_curve/cc5c0006-d328-443d-b742-f6650fdd9502|title=HV 2112 light curve|publisher=[[ASAS-SN]]|accessdate=2017-07-12}}
*{{cite web|url=https://asas-sn.osu.edu/light_curve/cc5c0006-d328-443d-b742-f6650fdd9502|title=HV 2112 light curve|publisher=[[ASAS-SN]]|access-date=2017-07-12}}{{Dead link|date=March 2023 |bot=InternetArchiveBot |fix-attempted=yes }}
*{{cite web|url=http://www.sci-news.com/astronomy/science-thorne-zytkow-object-01970.html|title=First Thorne-Zytkow Object Found 200,000 Light-Years Away|date=5 June 2014|accessdate=30 June 2014}}
*{{cite web|url=http://www.sci-news.com/astronomy/science-thorne-zytkow-object-01970.html|title=First Thorne-Zytkow Object Found 200,000 Light-Years Away|date=5 June 2014|access-date=30 June 2014}}
*{{cite web|url=http://phys.org/news/2014-06-kip-thorne-discusses-discovery-thorne-zytkow.html|title=Kip Thorne discusses first discovery of Thorne-Zytkow object|last=Eller|first=Cynthia|date=30 June 2014|accessdate=30 June 2014}}
*{{cite web|url=http://phys.org/news/2014-06-kip-thorne-discusses-discovery-thorne-zytkow.html|title=Kip Thorne discusses first discovery of Thorne-Zytkow object|last=Eller|first=Cynthia|date=30 June 2014|access-date=30 June 2014}}


{{Stars of Tucana}}
{{Stars of Tucana}}


{{DEFAULTSORT:HV 2112}}
[[Category:Stars in the Small Magellanic Cloud]]
[[Category:Stars in the Small Magellanic Cloud]]
[[Category:Tucana (constellation)]]
[[Category:Tucana]]
[[Category:Small Magellanic Cloud]]
[[Category:M-type bright giants]]
[[Category:M-type bright giants]]
[[Category:Mira variables]]
[[Category:Mira variables]]
[[Category:2MASS objects]]
[[Category:2MASS objects|J01100385-7236526]]
[[Category:Emission-line stars]]
[[Category:Emission-line stars]]
[[Category:Extragalactic stars]]
[[Category:Extragalactic stars]]
[[Category:PMMR objects]]
[[Category:TIC objects]]
[[Category:Asymptotic-giant-branch stars]]

Latest revision as of 17:34, 3 October 2024

HV 2112
HV-2112
HV 2112 (circled in red)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Tucana
Right ascension 01h 10m 03.858s[1]
Declination −72° 36′ 52.62″[1]
Apparent magnitude (V) 12.7 to below 16.7[2][3]
Characteristics
Spectral type M5.5 II (M3e – M7.5[4])
Apparent magnitude (J) 10.020[1]
Apparent magnitude (H) 9.100[1]
Apparent magnitude (K) 8.723[1]
U−B color index +0.33[5]
B−V color index +1.80[5]
Variable type Mira?[6]
Astrometry
Radial velocity (Rv)157[7] km/s
Proper motion (μ) RA: 1.116±0.073[8] mas/yr
Dec.: −1.291±0.067[8] mas/yr
Parallax (π)−0.2029 ± 0.0446 mas[8]
Absolute magnitude (MV)−5.2[7]
Details
Mass~5[9] M☉
Radius675 - 1,193[9][a] R☉
Luminosity50,100 - 81,300[9] L☉
Surface gravity (log g)0.0[7] cgs
Temperature2,500 - 3,750[9] K
Metallicity [Fe/H]-2.18[10] dex
Other designations
HV 2112, 2MASS J01100385-7236526, SMC V2156,[6] PMMR 187[11]
Database references
SIMBADdata

HV 2112 is a cool luminous variable star in the Small Magellanic Cloud. Until 2018, it was considered to be the most likely candidate for a Thorne–Żytkow object, but it is now thought to be an asymptotic giant branch star.

Discovery

[edit]

HV 2112 was first reported as a variable star in 1908, by Henrietta Leavitt. At the time it was identified as Harvard no. 2112. No period was given, but it was reported to be "probably long". The magnitude range was given as 13.7 to fainter than 16.5, from photographic plates.[12]

In 1966, analysis of Magellanic Cloud variable stars showed that HV 2112 had a photographic magnitude range from 13.0 to below 17.8. It was classified as a long-period variable, now known as a Mira variable, on the basis of its large amplitude and reasonably regular light variations, with a period of about 600 days.[13][14]

Possible object types

[edit]
A visual band light curve for HV 2112, plotted from ASAS-SN data[15]

AGB star

[edit]

HV 2112 had historically been treated as a very luminous asymptotic giant branch (AGB) star, a red giant that has exhausted its core helium and is in the last stages of its evolution. Large-amplitude class-M variables and stars with spectral types later than about M5 are almost always AGB stars rather than red supergiants. These stars have a theoretical maximum luminosity and, at the distance of the SMC, HV 2112 was typically calculated to be slightly more luminous than this limit at around 60,000 L☉.[4]

More modern calculations gave higher values for the luminosity of HV 2112 above 100,000 L☉, which is unambiguously too luminous to be an AGB star. These calculations included an interstellar extinction value of 0.4 magnitudes which is higher than average for massive stars in the SMC. However, it is not exceptional for red supergiants, which are believed to show additional extinction due to circumstellar dust near the star.[7]

Analysis of the proper motion of HV 2112 in 2016 reported that it is unusually large for an SMC star, although the radial velocity is consistent with other SMC objects. The proper motion of around 10 mas/year would indicate a space velocity of 3,100 km/sec at the distance of the SMC, well above its escape velocity. A more likely explanation of such a proper motion would be that HV 2112 lies about 3,000 parsecs away in our own galaxy. It would then be around 1,000 L☉ rather than 100,000 L☉ and so a typical AGB star. The over-abundance of heavy elements would then be explained as pollution from an unseen companion, producing an extrinsic S-type star.[16] Other analyses of the proper motion show much smaller velocities, consistent with an object in the SMC[17][18]

Thorne–Żytkow object

[edit]

In 2014, HV 2112 was identified as a possible Thorne–Żytkow object (TZO) using the Magellan Clay telescope in Chile. To find candidate TZOs, Emily Levesque used the Apache Point Observatory to examine 24 red supergiant stars in the Milky Way, and the Magellan Clay telescope to look at 16 in the Large Magellanic Cloud and 22 in the Small Magellanic Cloud. The star was thought to contain unusually high levels of the elements lithium, molybdenum and rubidium that are expected only to be produced by TZOs.[7]

A 2018 paper re-appraising the properties of HV 2112 found no evidence for unusual chemical abundances and a luminosity that is lower than previously thought. This suggests that the star is unlikely to be a TZO, and is much more likely an intermediate mass AGB star.[9]

Binary star

[edit]

HV 2112 is listed in the OGLE catalogue as an unresolved multiple star. The proper motions and radial velocity are consistent with other SMC objects, while the parallax is negative but acceptably close to the expected value for such a distant object.[19]

See also

[edit]

References

[edit]
  1. ^ a b c d e Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  2. ^ Kochanek, C. S.; Shappee, B. J.; Stanek, K. Z.; Holoien, T. W.-S.; Thompson, Todd A.; Prieto, J.-L.; Dong, Subo; Shields, J. V.; Will, D.; et al. (2017). "The All-Sky Automated Survey for Supernovae (ASAS-SN) Light Curve Server v1.0". Publications of the Astronomical Society of the Pacific. 129 (980): 104502. arXiv:1706.07060. Bibcode:2017PASP..129j4502K. doi:10.1088/1538-3873/aa80d9. S2CID 118995322.
  3. ^ Shappee, B. J.; Prieto, J. L.; Grupe, D.; Kochanek, C. S.; Stanek, K. Z.; De Rosa, G.; Mathur, S.; Zu, Y.; Peterson, B. M.; et al. (2014). "The Man behind the Curtain: X-Rays Drive the UV through NIR Variability in the 2013 Active Galactic Nucleus Outburst in NGC 2617". The Astrophysical Journal. 788 (1): 48. arXiv:1310.2241. Bibcode:2014ApJ...788...48S. doi:10.1088/0004-637X/788/1/48. S2CID 119113433.
  4. ^ a b Wood, P. R.; Bessell, M. S.; Fox, M. W. (1983). "Long-period variables in the Magellanic Clouds – Supergiants, AGB stars, supernova precursors, planetary nebula precursors, and enrichment of the interstellar medium". Astrophysical Journal. 272: 99. Bibcode:1983ApJ...272...99W. doi:10.1086/161265.
  5. ^ a b Boyer, Martha L.; Srinivasan, Sundar; Van Loon, Jacco Th.; McDonald, Iain; Meixner, Margaret; Zaritsky, Dennis; Gordon, Karl D.; Kemper, F.; Babler, Brian; et al. (2011). "Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low Metallicity Small Magellanic Cloud (SAGE-SMC). II. Cool Evolved Stars". The Astronomical Journal. 142 (4): 103. arXiv:1106.5026. Bibcode:2011AJ....142..103B. doi:10.1088/0004-6256/142/4/103. S2CID 119268816.
  6. ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  7. ^ a b c d e Levesque, Emily (1 September 2014). "Discovery of a Thorne-̇Żytkow object candidate in the Small Magellanic Cloud". Monthly Notices of the Royal Astronomical Society: Letters. 443: L94–L98. arXiv:1406.0001. Bibcode:2014MNRAS.443L..94L. doi:10.1093/mnrasl/slu080. S2CID 119192926.
  8. ^ a b c Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  9. ^ a b c d e Beasor, Emma; Davies, Ben; Cabrera-Ziri, Ivan; Hurst, Georgia (2 July 2018). "A critical re-evaluation of the Thorne-Żytkow object candidate HV 2112". Monthly Notices of the Royal Astronomical Society. 479 (3): 3101. arXiv:1806.07399. Bibcode:2018MNRAS.479.3101B. doi:10.1093/mnras/sty1744. S2CID 67766043.
  10. ^ Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevič, G.; Monari, G.; Cantat-Gaudin, T.; Weiler, M.; Khan, S.; Miglio, A.; Carrillo, I.; Romero-Gómez, M.; Minchev, I.; De Jong, R. S.; Antoja, T.; Ramos, P.; Steinmetz, M.; Enke, H. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics. 628: A94. arXiv:1904.11302. Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765. S2CID 131780028.
  11. ^ "HV 2112". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-05-05.
  12. ^ Leavitt, Henrietta S. (1908). "1777 variables in the Magellanic Clouds". Annals of Harvard College Observatory. 60: 87. Bibcode:1907AnHar..60...87L.
  13. ^ Payne-Gaposchkin, Cecilia; Gaposchkin, Sergei (1966). "Variable Stars in the Small Magellanic Cloud". Smithsonian Contributions to Astrophysics. 9: 1–205. Bibcode:1966SCoA....9....1P. doi:10.5479/si.00810231.9.1.
  14. ^ O’Grady, Anna J. G.; Drout, Maria R.; Shappee, B. J.; Bauer, Evan B.; Fuller, Jim; Kochanek, C. S.; Jayasinghe, T.; Gaensler, B. M.; Stanek, K. Z.; Holoien, Thomas W. S.; Prieto, J. L.; Thompson, Todd A. (October 2020). "Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds from ASAS-SN: Implications for Thorne-Żytkow Objects and Super-asymptotic Giant Branch Stars". The Astrophysical Journal. 901 (2): 135. arXiv:2008.06563. Bibcode:2020ApJ...901..135O. doi:10.3847/1538-4357/abafad.
  15. ^ "ASAS-SN Variable Stars Database". ASAS-SN Variable Stars Database. ASAS-SN. Retrieved 6 January 2022.
  16. ^ MacCarone, Thomas J.; De Mink, Selma E. (2016). "Large proper motion of the Thorne-Żytkow object candidate HV 2112 reveals its likely nature as foreground Galactic S-star". Monthly Notices of the Royal Astronomical Society: Letters. 458 (1): L1. arXiv:1601.05455. Bibcode:2016MNRAS.458L...1M. doi:10.1093/mnrasl/slw004. S2CID 119306614.
  17. ^ Worley, C. Clare; Irwin, Mike. J.; Tout, Christopher A.; Żytkow, Anna N.; Fraser, Morgan; Izzard, Robert G. (2016). "The proper motion of HV2112: A TŻO candidate in the SMC". Monthly Notices of the Royal Astronomical Society: Letters. 459 (1): L31–L35. arXiv:1602.08479. Bibcode:2016MNRAS.459L..31W. doi:10.1093/mnrasl/slw034. S2CID 118463486.
  18. ^ McMillan, Paul J; Church, Ross P (2018). "Gaia DR2 confirms that candidate Thorne-Żytkow object HV 2112 is in the SMC". Research Notes of the AAS. 2 (2): 18. arXiv:1804.10192v1. Bibcode:2018RNAAS...2...18M. doi:10.3847/2515-5172/aac0fb. S2CID 125376171.
  19. ^ González-Fernández, Carlos; Dorda, Ricardo; Negueruela, Ignacio; Marco, Amparo (2015). "A new survey of cool supergiants in the Magellanic Clouds". Astronomy & Astrophysics. 578: A3. arXiv:1504.00003. Bibcode:2015A&A...578A...3G. doi:10.1051/0004-6361/201425362. S2CID 55959019.

Notes

[edit]
  1. ^ Calculated from effective temperature and luminosity figures, with reference to the nominal solar temperature of 5,772 K:
[edit]
Retrieved from "https://en.wikipedia.org/enwiki/w/index.php?title=HV_2112&oldid=1249187137"