Astronomy:V4332 Sagittarii

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V4332 Sagittarii
V4332SgrLightCurve.png
A visual band light curve for V4332 Sagittarii. The main plot, adapted from Tylenda et al. (2015),[1] shows the long-term variability, and the inset, adapted from Martini et al. (1999),[2] shows the variation during the first weeks of the eruption.
Observation data
Equinox J2000.0]] (ICRS)
Constellation Sagittarius
Right ascension  18h 50m 36.696s[3]
Declination –21° 23′ 28.93″[3]
Apparent magnitude (V) 8.5[2]
Characteristics
Spectral type K8/M0e[4]
Astrometry
Proper motion (μ) RA: −2.722[3] mas/yr
Dec.: −5.555[3] mas/yr
Parallax (π)0.0017 ± 0.2798[3] mas
Distance(3.71±3.3)×103[5] ly
Other designations
V4332 Sgr, Nova Sgr 1994[6]
Database references
SIMBADdata

V4332 Sagittarii is a nova-like event in the constellation of Sagittarius. It was discovered February 24, 1994 at an apparent visual magnitude of 8.9 by Japanese amateur astronomer Minoru Yamamoto from Okazaki, Aichi, then confirmed by K. Hirosawa.[7] Initially designated Nova Sagittarii 1994 #1, it was given the variable star designation V4332 Sgr.[2] A spectra of the event taken March 4 lacked the characteristic features of a classical nova, with the only emission lines being of the Balmer series.[8] Subsequent spectra showed a rapid decline in luminosity and a change of spectral type over a period of five days.[2] By 2003, the object was ~1500 times less luminous than at peak magnitude and showed a spectrum of an M-type star.[9]

The nova-like event V838 Mon and this outburst formed an unusual category of erupting stars. In 2003, N. Soker and R. Tylenda proposed an accretion scenario as an explanation. They noted that a merger of two main sequence stars in a close binary orbit could explain the observed properties,[10] a process now known as a luminous red nova. In this scenario, the decline in brightness and radius of V4332 Sgr was a consequence of the merged stellar envelope undergoing gravitational contraction.[9]

An infrared excess from the object suggests it has a circumstellar disk. The infrared spectrum of this feature showed an absorption band of water ice and a carbon monoxide emission band.[9] By 2010, the stellar component had become concealed by a dusty disk viewed edge-on.[1] This dust includes a significant component of alumina, with growing amounts of magnesia and iron oxide.[11]

See also

References

  1. ↑ 1.0 1.1 Tylenda, R. et al. (June 2015), "VLT/UVES spectroscopy of V4332 Sagittarii in 2005: The best view on a decade-old stellar-merger remnant", Astronomy & Astrophysics 578: 14, doi:10.1051/0004-6361/201425592, A75, Bibcode: 2015A&A...578A..75T. 
  2. ↑ 2.0 2.1 2.2 2.3 Martini, Paul et al. (August 1999), "Nova Sagittarii 1994 1 (V4332 Sagittarii): The Discovery and Evolution of an Unusual Luminous Red Variable Star", The Astronomical Journal 118 (2): 1034–1042, doi:10.1086/300951, Bibcode: 1999AJ....118.1034M. 
  3. ↑ 3.0 3.1 3.2 3.3 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  4. ↑ Kimeswenger, S. (January 2006), "V4332 Sgr in 'Quiescence'", Astronomische Nachrichten 327 (1): 44–52, doi:10.1002/asna.200510482, Bibcode: 2006AN....327...44K. 
  5. ↑ Özdönmez, Aykut et al. (September 2016), "The distances of the Galactic novae", Monthly Notices of the Royal Astronomical Society 461 (2): 1177–1201, doi:10.1093/mnras/stw1362, Bibcode: 2016MNRAS.461.1177O. 
  6. ↑ "V4332 Sgr". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V4332+Sgr. 
  7. ↑ Marsden, B. G., ed. (February 1994), "Nova Sagittarii 1994", IAU Circular 5942 (1): 1, Bibcode: 1994IAUC.5942....1H. 
  8. ↑ Wagner, R. M. et al. (March 1994), Marsden, B. G., ed., "Nova Sagittarii 1994", IAU Circular 5944 (1): 1, Bibcode: 1994IAUC.5944....1W. 
  9. ↑ 9.0 9.1 9.2 Tylenda, R. et al. (August 2005), "V4332 Sagittarii revisited", Astronomy and Astrophysics 439 (2): 651–661, doi:10.1051/0004-6361:20041581, Bibcode: 2005A&A...439..651T. 
  10. ↑ Soker, Noam; Tylenda, Romuald (January 2003), "Main-Sequence Stellar Eruption Model for V838 Monocerotis", The Astrophysical Journal 582 (2): L105–L108, doi:10.1086/367759, Bibcode: 2003ApJ...582L.105S. 
  11. ↑ Banerjee, Dipankar. P. K. et al. (December 2015), "Evolution of the Dust in V4332 Sagittarii", The Astrophysical Journal 814 (2): 9, doi:10.1088/0004-637X/814/2/109, 109, Bibcode: 2015ApJ...814..109B. 

Further reading

  • Goranskij, V. P. et al. (June 2018), "Rapid re-brightening of the red nova V4332 Sgr remnant", The Astronomer's Telegram 11733 (11733): 1, Bibcode: 2018ATel11733....1G. 
  • Kamiński, T.; Tylenda, R. (October 2013), "Optical spectropolarimetry of V4332 Sagittarii", Astronomy & Astrophysics 558: 7, doi:10.1051/0004-6361/201321852, A82, Bibcode: 2013A&A...558A..82K. 
  • Kamiński, T.; Tylenda, R. (March 2011), "Strong linear polarization of V4332 Sagittarii: a dusty disc geometry", Astronomy & Astrophysics 527: 3, doi:10.1051/0004-6361/201015950, A75, Bibcode: 2011A&A...527A..75K. 
  • Kamiński, T. et al. (November 2010), "V4332 Sagittarii: a circumstellar disc obscuring the main object", Astronomy and Astrophysics 522: 12, doi:10.1051/0004-6361/201014406, A75, Bibcode: 2010A&A...522A..75K. 
  • Banerjee, D. P. K. et al. (September 2007), "Spitzer Observations of V4332 Sagittarii: Detection of Alumina Dust", The Astrophysical Journal 666 (1): L25–L28, doi:10.1086/521528, Bibcode: 2007ApJ...666L..25B. 
  • Goranskij, V. et al. (August 2006), "Unexpected change in the spectrum of V4332 Sgr", The Astronomer's Telegram 876 (876): 1, Bibcode: 2006ATel..876....1G. 
  • Lynch, D. K. et al. (August 2006), Green, D. W. E., ed., "V4332 Sagittarii", IAU Circular 8739 (1): 1, Bibcode: 2006IAUC.8739....1L. 
  • Banerjee, Dipankar P. K. (June 2005), "Studies of the peculiar nova V4332 Sgr", Bulletin of the Astronomical Society of India 33 (2): 81, Bibcode: 2005BASI...33...81B. 
  • Banerjee, Dipankar P. K. et al. (November 2004), "L and M Band Infrared Studies of V4332 Sagittarii: Detection of the Water Ice Absorption Band at 3.05 μm and the CO Fundamental Band in Emission", The Astrophysical Journal 615 (1): L53–L56, doi:10.1086/425963, Bibcode: 2004ApJ...615L..53B. 
  • Banerjee, Dipankar P. K. et al. (July 2004), "A Search for Radioactive 26Al in the Nova-like Variable V4332 Sagittarii", The Astrophysical Journal 610 (1): L29–L32, doi:10.1086/423171, Bibcode: 2004ApJ...610L..29B. 
  • Banerjee, Dipankar P. K.; Ashok, Nagarhalli M. (March 2004), "Optical Studies of V4332 Sagittarii: Detection of Unusually Strong K I and Na I Lines in Emission", The Astrophysical Journal 604 (1): L57–L60, doi:10.1086/383264, Bibcode: 2004ApJ...604L..57B. 
  • Banerjee, Dipankar P. K. et al. (November 2003), "Remarkable Changes in the Near-Infrared Spectrum of the Nova-like Variable V4332 Sagittarii", The Astrophysical Journal 598 (1): L31–L34, doi:10.1086/380389, Bibcode: 2003ApJ...598L..31B. 



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