Y
YCVn
Guest
+discoverer of variability
[td]1963, p. 407.</ref> It has a [[luminosity]] of 927 times that of the [[Sun]] and a surface temperature of {{val|14,550|ul=K|fmt=commas}}. Merope's mass is roughly {{solar mass|4.25|link=y}} and has a radius 4.8 times as great as the Sun's.[/td] [td][/td]
[td][/td] [td]Merope is classified as a [[Beta Cephei variable]], a type of hot [[variable star]] which pulsates regularly due to opacity changes in its atmosphere. Its brightness varies by up to 0.01 magnitudes during each pulsation cycle.<ref name=gcvs/> It is given the [[variable star designation]] of '''V971 Tauri'''. The period of variability is stable at 0.49 days, although the amplitude of the brightness changes on each cycle varies.<ref name="White2017"/>[/td]
[td]In 1985, Bernard J. McNamara announced that the brightness of Merope varies as a function of time.<ref name="ApJ1985"/> Merope is classified as a [[Beta Cephei variable]], a type of hot [[variable star]] which pulsates regularly due to opacity changes in its atmosphere. Its brightness varies by up to 0.01 magnitudes during each pulsation cycle.<ref name=gcvs/> It is given the [[variable star designation]] of '''V971 Tauri'''. The period of variability is stable at 0.49 days, although the amplitude of the brightness changes on each cycle varies.<ref name="White2017"/>[/td] [td][/td]
[td][/td] [td]Some papers have reported a companion star to Merope, at a separation of {{val|250|ul=mas}}, as well as several other visual companions farther out. These possible companions have not been confirmed.<ref name=Hutter/>[/td]
[td]Some papers have reported a companion star to Merope, at a separation of {{val|250|ul=mas}}, as well as several other visual companions farther out. These possible companions have not been confirmed.<ref name=Hutter/>[/td] [td][/td]
[td][/td] [td]<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>[/td]
[td]<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>[/td] [td][/td] [td]<ref name="ApJ1985">{{cite journal |last1=McNamara |first1=B. J. |title=Maia variables and upper-main-sequence phenomena |journal=Astrophysical Journal |date=February 1985 |volume=289 |pages=213-219 |doi=10.1086/162881 |bibcode=1985ApJ...289..213M |url=https://articles.adsabs.harvard.edu/pdf/1985ApJ...289..213M |access-date=2 September 2025}}</ref>[/td] [td][/td]
[td][/td] [td]<ref name="White2017">{{cite journal |last1=White |first1=T. R. |last2=Pope |first2=B. J. S. |last3=Antoci |first3=V. |last4=Papics |first4=P. I. |last5=Aerts |first5=C. |last6=Gies |first6=D. R. |last7=Gordon |first7=K. |last8=Huber |first8=D. |last9=Schaefer |first9=G. H. |last10=Aigrain |first10=S. |last11=Albrecht |first11=S. |last12=Barclay |first12=T. |last13=Barentsen |first13=G. |last14=Beck |first14=P. G. |last15=Bedding |first15=T. R. |last16=Fredslund |first16=M. |last17=Andersen |first17=M. Fredslund |last18=Grundahl |first18=F. |last19=Howell |first19=S. B. |last20=Ireland |first20=M. J. |last21=Murphy |first21=S. J. |last22=Nielsen |first22=M. B. |last23=Aguirre |first23=V. Silva |last24=Tuthill |first24=P. G. |title=Beyond the Kepler/K2 bright limit: variability in the seven brightest members of the Pleiades |journal=Monthly Notices of the Royal Astronomical Society |date=November 2017 |volume=471 |issue=3 |pages=2882β2901 |doi=10.1093/mnras/stx1050 |arxiv=1708.07462 |bibcode=2017MNRAS.471.2882W |doi-access=free }}</ref>[/td]
[td]<ref name="White2017">{{cite journal |last1=White |first1=T. R. |last2=Pope |first2=B. J. S. |last3=Antoci |first3=V. |last4=Papics |first4=P. I. |last5=Aerts |first5=C. |last6=Gies |first6=D. R. |last7=Gordon |first7=K. |last8=Huber |first8=D. |last9=Schaefer |first9=G. H. |last10=Aigrain |first10=S. |last11=Albrecht |first11=S. |last12=Barclay |first12=T. |last13=Barentsen |first13=G. |last14=Beck |first14=P. G. |last15=Bedding |first15=T. R. |last16=Fredslund |first16=M. |last17=Andersen |first17=M. Fredslund |last18=Grundahl |first18=F. |last19=Howell |first19=S. B. |last20=Ireland |first20=M. J. |last21=Murphy |first21=S. J. |last22=Nielsen |first22=M. B. |last23=Aguirre |first23=V. Silva |last24=Tuthill |first24=P. G. |title=Beyond the Kepler/K2 bright limit: variability in the seven brightest members of the Pleiades |journal=Monthly Notices of the Royal Astronomical Society |date=November 2017 |volume=471 |issue=3 |pages=2882β2901 |doi=10.1093/mnras/stx1050 |arxiv=1708.07462 |bibcode=2017MNRAS.471.2882W |doi-access=free }}</ref>[/td]
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[td]
β Previous revision
[/td][td]
[td]1963, p. 407.</ref> It has a [[luminosity]] of 927 times that of the [[Sun]] and a surface temperature of {{val|14,550|ul=K|fmt=commas}}. Merope's mass is roughly {{solar mass|4.25|link=y}} and has a radius 4.8 times as great as the Sun's.[/td]Revision as of 22:50, 2 September 2025
[/td][td]1963, p. 407.</ref> It has a [[luminosity]] of 927 times that of the [[Sun]] and a surface temperature of {{val|14,550|ul=K|fmt=commas}}. Merope's mass is roughly {{solar mass|4.25|link=y}} and has a radius 4.8 times as great as the Sun's.[/td] [td][/td]
[td][/td] [td]Merope is classified as a [[Beta Cephei variable]], a type of hot [[variable star]] which pulsates regularly due to opacity changes in its atmosphere. Its brightness varies by up to 0.01 magnitudes during each pulsation cycle.<ref name=gcvs/> It is given the [[variable star designation]] of '''V971 Tauri'''. The period of variability is stable at 0.49 days, although the amplitude of the brightness changes on each cycle varies.<ref name="White2017"/>[/td]
[td]In 1985, Bernard J. McNamara announced that the brightness of Merope varies as a function of time.<ref name="ApJ1985"/> Merope is classified as a [[Beta Cephei variable]], a type of hot [[variable star]] which pulsates regularly due to opacity changes in its atmosphere. Its brightness varies by up to 0.01 magnitudes during each pulsation cycle.<ref name=gcvs/> It is given the [[variable star designation]] of '''V971 Tauri'''. The period of variability is stable at 0.49 days, although the amplitude of the brightness changes on each cycle varies.<ref name="White2017"/>[/td] [td][/td]
[td][/td] [td]Some papers have reported a companion star to Merope, at a separation of {{val|250|ul=mas}}, as well as several other visual companions farther out. These possible companions have not been confirmed.<ref name=Hutter/>[/td]
[td]Some papers have reported a companion star to Merope, at a separation of {{val|250|ul=mas}}, as well as several other visual companions farther out. These possible companions have not been confirmed.<ref name=Hutter/>[/td] [td][/td]
[td][/td] [td]<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>[/td]
[td]<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>[/td] [td][/td] [td]<ref name="ApJ1985">{{cite journal |last1=McNamara |first1=B. J. |title=Maia variables and upper-main-sequence phenomena |journal=Astrophysical Journal |date=February 1985 |volume=289 |pages=213-219 |doi=10.1086/162881 |bibcode=1985ApJ...289..213M |url=https://articles.adsabs.harvard.edu/pdf/1985ApJ...289..213M |access-date=2 September 2025}}</ref>[/td] [td][/td]
[td][/td] [td]<ref name="White2017">{{cite journal |last1=White |first1=T. R. |last2=Pope |first2=B. J. S. |last3=Antoci |first3=V. |last4=Papics |first4=P. I. |last5=Aerts |first5=C. |last6=Gies |first6=D. R. |last7=Gordon |first7=K. |last8=Huber |first8=D. |last9=Schaefer |first9=G. H. |last10=Aigrain |first10=S. |last11=Albrecht |first11=S. |last12=Barclay |first12=T. |last13=Barentsen |first13=G. |last14=Beck |first14=P. G. |last15=Bedding |first15=T. R. |last16=Fredslund |first16=M. |last17=Andersen |first17=M. Fredslund |last18=Grundahl |first18=F. |last19=Howell |first19=S. B. |last20=Ireland |first20=M. J. |last21=Murphy |first21=S. J. |last22=Nielsen |first22=M. B. |last23=Aguirre |first23=V. Silva |last24=Tuthill |first24=P. G. |title=Beyond the Kepler/K2 bright limit: variability in the seven brightest members of the Pleiades |journal=Monthly Notices of the Royal Astronomical Society |date=November 2017 |volume=471 |issue=3 |pages=2882β2901 |doi=10.1093/mnras/stx1050 |arxiv=1708.07462 |bibcode=2017MNRAS.471.2882W |doi-access=free }}</ref>[/td]
[td]<ref name="White2017">{{cite journal |last1=White |first1=T. R. |last2=Pope |first2=B. J. S. |last3=Antoci |first3=V. |last4=Papics |first4=P. I. |last5=Aerts |first5=C. |last6=Gies |first6=D. R. |last7=Gordon |first7=K. |last8=Huber |first8=D. |last9=Schaefer |first9=G. H. |last10=Aigrain |first10=S. |last11=Albrecht |first11=S. |last12=Barclay |first12=T. |last13=Barentsen |first13=G. |last14=Beck |first14=P. G. |last15=Bedding |first15=T. R. |last16=Fredslund |first16=M. |last17=Andersen |first17=M. Fredslund |last18=Grundahl |first18=F. |last19=Howell |first19=S. B. |last20=Ireland |first20=M. J. |last21=Murphy |first21=S. J. |last22=Nielsen |first22=M. B. |last23=Aguirre |first23=V. Silva |last24=Tuthill |first24=P. G. |title=Beyond the Kepler/K2 bright limit: variability in the seven brightest members of the Pleiades |journal=Monthly Notices of the Royal Astronomical Society |date=November 2017 |volume=471 |issue=3 |pages=2882β2901 |doi=10.1093/mnras/stx1050 |arxiv=1708.07462 |bibcode=2017MNRAS.471.2882W |doi-access=free }}</ref>[/td]
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