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GT Muscae

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GT Muscae

Light curvesfor GT Muscae. The upper panel (adapted from Murdochet al.[1]) shows the long-term variability after a model of the eclipsing binary variability has been removed. The orbital period of HD 101379 is shown in red. The lower panel showsTESSdata,[2]in which the eclipses (both primary and secondary) are clearly visible. The orbital period of HD 101380 is shown in red.
Observation data
EpochJ2000.0EquinoxJ2000.0
Constellation Musca
Right ascension 11h39m29.56610s[3]
Declination −65° 23′ 52.0995″[3]
Apparent magnitude(V) 4.96 - 5.23[4]
Characteristics
Spectral type A: G5/8III+F, B: A0V+A2V[4]
Variable type Algol+RS CVn[5]
Astrometry
Proper motion(μ)RA:−29.762±0.561[3]mas/yr
Dec.:5.783±0.504[3]mas/yr
Parallax(π)8.3972 ± 0.5075mas[3]
Distance390 ± 20ly
(119 ± 7pc)
Orbit[6]
PrimaryA (HD 101379)
CompanionB (HD 101380)
Period(P)96.8±2.4yr
Semi-major axis(a)0.276″±0.004″
Eccentricity(e)0.634±0.015
Inclination(i)60.9±2°
Longitude of the node(Ω)259.8±1.5°
Periastronepoch(T)2452778±110
Argument of periastron(ω)
(secondary)		92.4±1.5°
Orbit[1]
PrimaryAa
CompanionAb
Period(P)61.448±0.007d
Periastronepoch(T)2444929±6
Argument of periastron(ω)
(secondary)		238±24°
Semi-amplitude(K1)
(primary)		12.7±0.2km/s
Orbit[4]
PrimaryBa
CompanionBb
Period(P)2.75459d
Details[7]
A
Mass1.1±0.3M☉
Radius16.6±1R☉
Luminosity126L☉
Surface gravity(logg)1.89±0.05cgs
Temperature4,744±125K
Other designations
12 Muscae,HD101379,HD101380,HIP56862,HR4492,SAO251522,WDSJ11395-6524AB,[8]B 1705 AB[9]
Database references
SIMBADdata

GT Muscae,also known as12 Muscae,is avariable starabout 400light yearsfrom the Earth, in the constellationMusca.[3]It is a 5thmagnitudestar, so it should be faintly visible to the naked eye of an observer far fromcity lights.[3]It is a quadruple star system, consisting of aspectroscopic binarycontaining anRS Canum Venaticorum variable(RS CVn) star (HD 101379), orbiting aneclipsing binary(HD 101380).[1]It varies in brightness from magnitude 4.96 to 5.23.[4]GT Muscae is a very activeX-raysource.[10]

In 1929,Willem van den Bosdiscovered that GT Muscae is a visualdouble star,whose A (HD 101379) and B (HD 101380) components were separated by 0.2arc secondsat the time he observed it.[9]Examiningphotographic platesin 1964, Wolfgang Strohmeieret al.discovered that GT Muscae is a variable star.[11]In 1979, based onspectroscopicfeatures, Edward Weiler and Robert Stencel listed GT Muscae as a likely RS CVn variable.[12]Eclipses of the HD 101380 pair were first reported byAndrew Collier Cameronin his 1982 PhD thesis, in which he also determined that pair's orbital period.[13]The entire star system was given thevariable star designationGT Muscae in 1988.[14]

Strong, variable, 5 GHz radio emission from GT Muscae, indicative offlares,was detected in 1982 and was interpreted as indicating high levels ofchromosphericandcoronalactivity.[15]

GT Muscae was detected in the early observations of theUhuruX-ray satellite, originally denoted as 2U 1134–161, later renamed 4U 1137–65.[16][17]Michael Garciaet al.identified HD 101379 as the source seen byUhuru,in 1980.[18]During the 2010-2019 decade, GT Muscae showed the most X-ray flare activity of any star in the sky, producing flares with energies as high as ~1038ergs.[10]

References

[edit]
  1. ^abcMurdoch, K. A.; Hearnshaw, J. B.; Kilmartin, P. M.; Gilmore, A. C. (October 1995)."A photometric and orbital analysis of GT Muscae".Monthly Notices of the Royal Astronomical Society.276(3): 836–846.Bibcode:1995MNRAS.276..836M.doi:10.1093/mnras/276.3.836.Retrieved26 January2023.
  2. ^"MAST: Barbara A. Mikulski Archive for Space Telescopes".Space Telescope Science Institute.Retrieved24 January2023.
  3. ^abcdefgVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData Release 3. Summary of the content and survey properties ".Astronomy and Astrophysics.674:A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
  4. ^abcd"GT Mus".The International Variable Star Index.AAVSO.Retrieved26 January2023.
  5. ^Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017)."General catalogue of variable stars: Version GCVS 5.1".Astronomy Reports.61(1): 80.Bibcode:2017ARep...61...80S.doi:10.1134/S1063772917010085.S2CID125853869.
  6. ^"11395-6524 B 1705AB (GT Mus)".Washington Double Star Catalog.US Naval Observatory.Retrieved28 January2023.
  7. ^Kallinger, T.; Beck, P. G.; Hekker, S.; Huber, D.; Kuschnig, R.; Rockenbauer, M.; Winter, P. M.; Weiss, W. W.; Handler, G.; Moffat, A. F. J.; Pigulski, A.; Popowicz, A.; Wade, G. A.; Zwintz, K. (2019-04-01). "Stellar masses from granulation and oscillations of 23 bright red giants observed by BRITE-Constellation".Astronomy & Astrophysics.624:A35.arXiv:1902.07531.Bibcode:2019A&A...624A..35K.doi:10.1051/0004-6361/201834514.ISSN0004-6361.
  8. ^"12 Mus -- RS CVn Variable".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2023-01-26.
  9. ^abvan den Bos, W. H. (October 1929)."New southern double stars, ninth list".Bulletin of the Astronomical Institutes of the Netherlands.5:125–134.Bibcode:1929BAN.....5..125V.Retrieved27 January2023.
  10. ^abSasaki, Ryo; Tsuboi, Yohko; Iwakiri, Wataru; Nakahira, Satoshi; Maeda, Yoshitomo; Gendreau, Keith; Corcoran, Michael F.; Hamaguchi, Kenji; Arzoumanian, Zaven; Markwardt, Craig B.; Enoto, Teruaki; Sato, Tatsuki; Kawai, Hiroki; Mihara, Tatehiro; Shidatsu, Megumi; Negoro, Hitoshi; Serino, Motoko (March 2021)."The RS CVn-type Star GT Mus Shows Most Energetic X-Ray Flares Throughout the 2010s".The Astrophysical Journal.910(1): 25.arXiv:2103.16822.Bibcode:2021ApJ...910...25S.doi:10.3847/1538-4357/abde38.S2CID232427851.
  11. ^Strohmeier, W.; Knigge, R.; Ott, H. (September 1964)."Bright Southern BV-Stars".Information Bulletin on Variable Stars.66(1): 1.Bibcode:1964IBVS...66....1S.Retrieved27 January2023.
  12. ^Weiler, E. J.; Stencel, R. E. (September 1979)."Southern RS CVn systems. Candidate list".Astronomical Journal.84:1372–1373.Bibcode:1979AJ.....84.1372W.doi:10.1086/112553.Retrieved27 January2023.
  13. ^Collier Cameron, Andrew (1982).Late-type Ca II emission-line stars in the Southern Hemisphere.University of Canterbury.Bibcode:1982PhDT.......163C.doi:10.26021/7260.Retrieved28 January2023.
  14. ^Kholopov, P. N.; Samus, N. N.; Kazarovets, B. V.; Frolov, M. S.; Kireeva, N. N. (April 1989)."The 69th Name-List of Variable Stars"(PDF).Information Bulletin on Variable Stars.3323(1): 1.Bibcode:1989IBVS.3323....1K.Retrieved27 January2023.
  15. ^Collier, A. C.; Haynes, R. F.; Slee, O. B.; Wright, A. E.; Hillier, D. J. (September 1982)."A coordinated radio and Half survey of southern RS CVn systems and related objects".Monthly Notices of the Royal Astronomical Society.200(4): 869–880.Bibcode:1982MNRAS.200..869C.doi:10.1093/mnras/200.4.869.Retrieved28 January2023.
  16. ^Giacconi, R.; Murray, S.; Gursky, H.; Kellogg, E.; Schreier, E.; Tananbaum, H. (December 1972)."The Uhuru catalog of X-ray sources".Astrophysical Journal.178:281–308.Bibcode:1972ApJ...178..281G.doi:10.1086/151790.Retrieved27 January2023.
  17. ^Forman, W.; Jones, C.; Cominsky, L.; Julien, P.; Murray, S.; Peters, G.; Tananbaum, H.; Giacconi, R. (December 1978)."The fourth Uhuru catalog of X-ray sources".Astrophysical Journal Supplement Series.38:357–412.Bibcode:1978ApJS...38..357F.doi:10.1086/190561.
  18. ^Garcia, M.; Baliunas, S. L.; Conroy, M.; Johnston, M. D.; Ralph, E.; Roberts, W.; Schwartz, D. A.; Tonry, J. (September 1980)."Optical identification of H 0123+07.5 and 4U 1137-65: hard X-ray emission from RS CVn systems".Astrophysical Journal.240:L107–L110.Bibcode:1980ApJ...240L.107G.doi:10.1086/183334.Retrieved28 January2023.
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