Astronomy:VX Sagittarii

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Short description: Asymptotic giant branch star in the constellation Sagittarius
VX Sagittarii
Observation data
Equinox J2000.0]] (ICRS)
Constellation Sagittarius
Right ascension  18h 08m 04.04831s[1]
Declination −22° 13′ 26.6327″[1]
Apparent magnitude (V) 6.5 - 14.0[2]
Characteristics
Evolutionary stage AGB, (possibly TŻO)[3]
Spectral type M4eIa - M10eIa[4]
Apparent magnitude (U) 11.72
Apparent magnitude (B) 9.41
Apparent magnitude (V) 6.52
Apparent magnitude (I) 2.11
Apparent magnitude (J) 1.23
Apparent magnitude (H) 0.13
Apparent magnitude (K) −0.50
Apparent magnitude (L) −1.61
Variable type SRc[2]
Astrometry
Radial velocity (Rv)+6.47±3.37[5] km/s
Proper motion (μ) RA: +0.36±0.76[5] mas/yr
Dec.: −2.92±0.78[5] mas/yr
Parallax (π)0.64 ± 0.04[5] mas
Distance5,100 ± 300 ly
(1,560 ± 100 pc)
Details
Mass12[6] M☉
Radius1,356,[3] between 1,120 and 1,550[5], 1,350–1,940 (pulsation)[7] R☉
Luminosity195000±62000[5], 110,000–190,000[7] L☉
Temperature2,900[8] (near min), 3,200-3,400 (near max)[6], 2,400–3,300[7] K
Other designations
VX Sgr, HIP 88838, BD−22°4575, CD−22°12589, HD 165674, 2MASS J18080404-2213266, AAVSO 1802-22
Database references
SIMBADdata

VX Sagittarii is an asymptotic giant branch star located more than 1.5 kiloparsec away from the Sun in the constellation of Sagittarius. It is a pulsating variable star with an unusually large magnitude range. It is one of the largest stars discovered, with a radius varying between 1,350 and 1,940 solar radii (940,000,000 and 1.35×109 km; 6.3 and 9.0 astronomical unit|au). It is the most luminous known AGB star, at bolometric magnitude –8.6, which is brighter than the theoretical limit at –8.0.[3]

Observations

A visual band light curve for VX Sagittarii, plotted from AAVSO data[9]

The star is classed as a cool semiregular variable of type SRc with a pulsational period of 732 days. The variations sometimes have an amplitude comparable to a long period variable, at other times they are much smaller. The spectral type varies between M4e around visual maximum and M9.8e at minimum light, and the luminosity class is Ia indicating a bright supergiant. The spectrum shows emission lines indicating that the star is losing mass through a strong stellar wind.[7]

The annual parallax of VX Sagittarii has been measured as 0.64±0.06 mas, indicating a distance of about 5,100 light years. This is compatible with the distance to Sagittarius OB1, the stellar association that VX Sagittarii is thought to belong to. Its radial velocity and proper motions are also consistent with other members of the association.[5]

Stellar characteristics

The effective temperature of VX Sagittarii is variable from around 2,400 K at visual minimum to around 3,300 K near maximum. Such low temperatures are comparable to the very coolest AGB stars and unprecedented for a massive supergiant.[6][7] Its atmosphere is extended, irregular, and variable during the pulsations of the star, but the bolometric luminosity varies less than the visual brightness and is calculated to be about 195,000 L☉. At an effective temperature of 3,300 K, the radius is expected to be somewhere between 1,120 R☉ and 1,550 R☉.[5] Older studies frequently calculated higher luminosities.[10][11]

The atmosphere of VX Sgr shows molecular water layers and SiO masers in the atmosphere, typical of an OH/IR star.[12] The masers have been used to derive a distance of 1,590 parsecs.[13] The spectrum also indicates strong VO and CN. In many respects the atmosphere is similar to low mass AGB stars such as Mira variables, but with a supergiant's luminosity and size.[6]

Another paper from May 2018 suggests that VX Sagitarii may be a hypergiant.[5] This would make it one of the very rare red hypergiant stars.

More recent[when?] papers state that VX Sagittarii is a massive AGB star, rather than a red supergiant or hypergiant. Because it displays rubidium in its spectrum and has a high mass loss and luminosity, it is possible that it is a type of AGB star known as a super-AGB star, a type of star with masses in between low-mass stars and high-mass stars.[3]

See also

References

  1. ↑ 1.0 1.1 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 Samus, N. N. 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. 
  3. ↑ 3.0 3.1 3.2 3.3 Tabernero, H. M.; Dorda, R.; Negueruela, I.; Marfil, E. (2021). "The nature of VX Sagitarii". Astronomy & Astrophysics 646: A98. doi:10.1051/0004-6361/202039236. 
  4. ↑ Kiss, L. L.; Szabó, G. M.; Bedding, T. R. (2006). "Variability in red supergiant stars: Pulsations, long secondary periods and convection noise". Monthly Notices of the Royal Astronomical Society 372 (4): 1721–1734. doi:10.1111/j.1365-2966.2006.10973.x. Bibcode: 2006MNRAS.372.1721K. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 5.8 Xu, Shuangjing; Zhang, Bo; Reid, Mark J; Menten, Karl M; Zheng, Xingwu; Wang, Guangli (2018). "The Parallax of the Red Hypergiant VX Sgr with Accurate Tropospheric Delay Calibration". The Astrophysical Journal 859 (1): 14. doi:10.3847/1538-4357/aabba6. Bibcode: 2018ApJ...859...14X. 
  6. ↑ 6.0 6.1 6.2 6.3 Chiavassa, A.; Lacour, S.; Millour, F.; Driebe, T.; Wittkowski, M.; Plez, B.; Thiébaut, E.; Josselin, E. et al. (2009). "VLTI/AMBER spectro-interferometric imaging of VX Sgr's inhomogenous outer atmosphere". Astronomy and Astrophysics 511: A51. doi:10.1051/0004-6361/200913288. Bibcode: 2010A&A...511A..51C. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Lockwood, G.W.; Wing, R. F. (1982). "The light and spectrum variations of VX Sagittarii, an extremely cool supergiant". Monthly Notices of the Royal Astronomical Society 198 (2): 385–404. doi:10.1093/mnras/198.2.385. Bibcode: 1982MNRAS.198..385L. 
  8. ↑ García-Hernández, D. A; García-Lario, P; Plez, B; Manchado, A; d'Antona, F; Lub, J; Habing, H (2007). "Lithium and zirconium abundances in massive Galactic O-rich AGB stars". Astronomy and Astrophysics 462 (2): 711. doi:10.1051/0004-6361:20065785. Bibcode: 2007A&A...462..711G. 
  9. ↑ "Download Data". AAVSO. https://www.aavso.org/data-download. 
  10. ↑ De Jager, C.; Nieuwenhuijzen, H.; Van Der Hucht, K. A. (1988). "Mass loss rates in the Hertzsprung-Russell diagram". Astronomy and Astrophysics Supplement Series 72: 259. Bibcode: 1988A&AS...72..259D. 
  11. ↑ Nicolas Mauron; Eric Josselin (2010). "The mass-loss rates of red supergiants and the de Jager prescription". Astronomy & Astrophysics 526: A156. doi:10.1051/0004-6361/201013993. Bibcode: 2011A&A...526A.156M. 
  12. ↑ Greenhill et al. (1995). "The SiO Masers and Dust Shell of VX SGR". Astrophysics and Space Science 224 (1–2): 1–9. doi:10.1007/BF00667909. Bibcode: 1995Ap&SS.224..469G. 
  13. ↑ Chen, X.; Shen, Z. Q.; Xu, Y. (2007). "Measuring the Distance of VX Sagittarii with SiO Maser Proper Motions". Chinese Journal of Astronomy and Astrophysics 7 (4): 531. doi:10.1088/1009-9271/7/4/09. Bibcode: 2007ChJAA...7..531C. 

Further reading

  • Chiavassa, A. et al. (February 2022), "The extended atmosphere and circumstellar environment of the cool evolved star VX Sagittarii as seen by MATISSE", Astronomy & Astrophysics 658: A185, doi:10.1051/0004-6361/202142514, A185, Bibcode: 2022A&A...658A.185C. 
  • Su, Jiang-Bo et al. (December 2020), "Observational characteristics of SiO masers around VX Sgr", Research in Astronomy and Astrophysics 20 (12): 192, doi:10.1088/1674-4527/20/12/192, 192, Bibcode: 2020RAA....20..192S. 
  • Su, J. B. et al. (January 2018), "Dynamics of SiO Masers around VX Sgr", The Astrophysical Journal 853 (1): 42, doi:10.3847/1538-4357/aaa12b, 42, Bibcode: 2018ApJ...853...42S. 
  • Su, J. B. et al. (September 2014), "Outward Motions of SiO Masers around VX Sgr", Journal of Astrophysics and Astronomy 35 (3): 539–540, doi:10.1007/s12036-014-9280-2, Bibcode: 2014JApA...35..539S. 
  • Su, J. B. et al. (July 2012), "High-resolution VLBA Observations of Three 7 mm SiO Masers toward VX Sgr at Five Epochs", The Astrophysical Journal 754 (1): 47, doi:10.1088/0004-637X/754/1/47, 47, Bibcode: 2012ApJ...754...47S. 
  • Su, J. B. et al. (June 2011), "Pumping Mechanisms for SiO Masers around VX Sgr", Journal of Astrophysics and Astronomy 32 (1–2): 261–264, doi:10.1007/s12036-011-9002-y, Bibcode: 2011JApA...32..261S. 
  • Lu, R. -S. et al. (2010), "High-frequency VLBI Imaging of Sgr A* and VX Sgr", Proceedings of the 10th European VLBI Network Symposium and EVN Users Meeting: VLBI and the new generation of radio arrays. September 20-24, 2010. Manchester, UK 10: p. 087, doi:10.22323/1.125.0087, 87, Bibcode: 2010evn..confE..87L. 
  • Chen, Xi et al. (April 2006), "Inward Motions of the Compact SiO Masers around VX Sagittarii", The Astrophysical Journal 640 (2): 982–994, doi:10.1086/500168, Bibcode: 2006ApJ...640..982C. 
  • Kamohara, Ryuichi et al. (April 2005), "Time Variation of SiO Masers in VX Sagittarii over an Optically Quiescent Phase", Publications of the Astronomical Society of Japan 57 (2): 341–345, doi:10.1093/pasj/57.2.341, Bibcode: 2005PASJ...57..341K. 
  • Murakawa, K. et al. (September 2003), "The radially expanding molecular outflow of VX Sagittarii", Monthly Notices of the Royal Astronomical Society 344 (1): 112, doi:10.1046/j.1365-8711.2003.06626.x, Bibcode: 2003MNRAS.344....1M. 
  • Yates, J. A. et al. (2002), Mineese, Victor; Reid, Mark, eds., "The H2O maser proper motions of RT Vir and VX Sgr", Cosmic Masers: From Proto-Stars to Black Holes, IAU Symposium #206, held 5-10 March 2001 in Angra dos Reis, Rio de Janeiro, Brazil (San Francisco: Astronomical Society of the Pacific) 206: p. 298, Bibcode: 2002IAUS..206..298Y. 
  • Szymczak, M. et al. (June 2001), "Magnetic field structure in the outer OH maser envelope of VX Sagittarii", Astronomy and Astrophysics 371 (3): 1012–1017, doi:10.1051/0004-6361:20010451, Bibcode: 2001A&A...371.1012S. 
  • Pashchenko, M. I.; Rudnitskii, G. M. (May 1999), "Observations of late-type variable stars in the water-vapor radio line. The supergiant VX Sagittarii", Astronomy Reports 43 (5): 311–324, Bibcode: 1999ARep...43..311P. 
  • Berulis, I. I. et al. (1999), "H2O maser emission of the M-type supergiant VX Sgr", Astronomical and Astrophysical Transactions 18 (1): 77–82, doi:10.1080/10556799908203038, Bibcode: 1999A&AT...18...77B. 
  • Trigilio 7, C. et al. (June 1998), "The circumstellar magnetic field of VX Sagittarii", Monthly Notices of the Royal Astronomical Society 297 (2): 497–501, doi:10.1046/j.1365-8711.1998.01538.x, Bibcode: 1998MNRAS.297..497T. 
  • Doeleman, S. S. et al. (1998), Zensus, J. A.; Taylor, G. B.; Wrobel, J. M., eds., "86 GHz VLBI Imaging of the SiO Masers in VX SGR", Radio Emission from Galactic and Extragalactic Compact Sources, IAU Colloquium 164, ASP Conference Series 144: p. 363, Bibcode: 1998ASPC..144..363D. 
  • Zell, Philip J.; Fix, John D. (July 1996), "The Spatial Distribution of Circularly Polarized 1612 MHz OH Maser Emission From VX SGR", Astronomical Journal 112: 252, doi:10.1086/118007, Bibcode: 1996AJ....112..252Z. 
  • Trigilio, C. et al. (1996), Pallavicini, Roberto; Dupree, Andrea K., eds., "Magnetic field measurements in the circumstellar envelope of VX SGR", Cool stars, stellar systems, and the sun: Proceedings of the 9th Cambridge workshop; held 3-6 October 1995 in Florence, Italy, Astronomical Society of the Pacific Conference Series (San Francisco: Astronomical Society of the Pacific) 109: p. 549, Bibcode: 1996ASPC..109..549T. 
  • Greenhill, Lincoln J. et al. (June 1994), Breckinridge, James B., ed., "Circumstellar envelope of VX SGR resolved with long-baseline interferometry at millimeter and midinfrared wavelengths", Conference Proceedings of SPIE: Amplitude and Intensity Spatial Interferometry II, Amplitude and Intensity Spatial Interferometry II 2200: pp. 304–315, doi:10.1117/12.177248, Bibcode: 1994SPIE.2200..304G. 
  • Greenhill, L. J. et al. (May 1993), "The Circumstellar Envelope of VX SGR", Bulletin of the American Astronomical Society 25: 824, Bibcode: 1993AAS...182.2203G. 
  • Yu, Zhiyao (June 1992), "The Circumstellar Envelope of VX-Sagittarii", Astrophysics and Space Science 192 (1): 53–62, doi:10.1007/BF00653259, Bibcode: 1992Ap&SS.192...53Y. 
  • Pijpers, F. P. (November 1990), "A model for the wind of the M supergiant VX Sagittarii", Astronomy and Astrophysics 238: 256, Bibcode: 1990A&A...238..256P. 
  • Netzer, Nathan (July 1989), "Interaction of Dust and Radiation in Circumstellar Envelopes. I. The Expansion Velocity Gradient in the Envelope of VX Sagittarii", Astrophysical Journal 342: 1068, doi:10.1086/167663, Bibcode: 1989ApJ...342.1068N. 
  • Chapman, J. M.; Cohen, R. J. (May 1986), "MERLIN observations of the circumstellar envelope of VX Sagittarius", Monthly Notices of the Royal Astronomical Society 220 (3): 513–528, doi:10.1093/mnras/220.3.513, Bibcode: 1986MNRAS.220..513C. 
  • Smith, Horace A. (February 1978), "Beat Phenomena in the Light Curve of VX Sgr", The Journal of the American Association of Variable Star Observers 6 (2): 63, Bibcode: 1978JAVSO...6...63S. 
  • Dinerstein, Harriet (1973), "VX Sagittarii: A Variable at Many Wavelengths", Journal of the American Association of Variable Star Observers 2 (2): 52–59, Bibcode: 1973JAVSO...2...52D. 
  • Humphreys, Roberta M.; Lockwood, G. W. (March 1972), "Spectroscopic and Photometric Changes in the Peculiar Infrared Star VX Sagittarius", Astrophysical Journal 172: L59, doi:10.1086/180891, Bibcode: 1972ApJ...172L..59H. 
  • Robinson, B. J. et al. (March 1971), "Similarity of the OH Emissions from VX Sagittarii and VY Canis Majoris", Astrophysical Letters 8: 171, Bibcode: 1971ApL.....8..171R. 




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