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
Epoch J2000.0       Equinox J2000.0
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  mas/yr [3]
Dec.: −5.555  mas/yr [3]
Parallax (π)0.0017 ± 0.2798  mas [3]
Distance (3.71±3.3)×103 [5]   ly
Other designations
V4332 Sgr, Nova Sgr 1994 [6]
Database references
SIMBAD data

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]

Contents

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

Related Research Articles

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<span class="mw-page-title-main">W Sagittarii</span> Star in the constellation Sagittarius

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<span class="mw-page-title-main">Tau Sagittarii</span> Orange-hued giant star in the constellation Sagittarius

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Xi<sup>2</sup> Sagittarii Star in the constellation Sagittarius

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Xi<sup>1</sup> Sagittarii Star in the constellation Sagittarius

Xi1 Sagittarii (ξ1 Sagittarii) is a solitary, blue-white hued star in the zodiac constellation of Sagittarius. It is visible to the naked eye with an apparent visual magnitude of +5.06. Based upon a small annual parallax shift of 1.58 mas as seen from Earth, this system is located roughly 2,100 light years from the Sun.

<span class="mw-page-title-main">Omicron Sagittarii</span> Star in the constellation Sagittarius

ο Sagittarii, Latinized as Omicron Sagittarii, is a single star in the constellation Sagittarius. It is yellow in hue and visible to the naked eye with an apparent visual magnitude of +3.77. The distance to this star is approximately 142 light years based on parallax. It is drifting further away from the Sun with a radial velocity of +26 km/s, having come to within 86 ly around a million years ago.

<span class="mw-page-title-main">Iota Sagittarii</span> Astrometric binary star in the constellation Sagittarius

Iota Sagittarii is a star in the zodiac constellation of Sagittarius. With an apparent visual magnitude of +4.118, it is bright enough to be viewed with the naked eye. Based upon an annual parallax shift of 17.94 mas as seen from Earth, this star is located 182 light years from the Sun. It is moving away from the Earth with a radial velocity of +35.8 km/s.

<span class="mw-page-title-main">60 Sagittarii</span> Possible binary star system in the constellation Sagittarius

60 Sagittarii is a suspected binary star system in the southern constellation of Sagittarius. It has the Bayer designation A Sagittarii, while 60 Sagittarii is the Flamsteed designation. This naked-eye object forms the northwest corner of the asterism called the Terebellum and, with an apparent magnitude of approximately 4.84, it is the dimmest of the four stars in the Terebellum. It is located 379 light-years from the Sun, based on parallax, but is moving closer with a radial velocity of −51 km/s.

<span class="mw-page-title-main">X Sagittarii</span> Variable star and possible binary star system in the constellation Sagittarius

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Nu<sup>1</sup> Sagittarii Triple star system in the constellation Sagittarius

Nu¹ Sagittarii is a triple star system about 1,100 light-years from Earth. Its three components are designated Nu¹ Sagittarii A, B and C. A and B themselves form a spectroscopic binary. The system is 0.11 degree north of the ecliptic.

<span class="mw-page-title-main">Psi Sagittarii</span> Triple star system in the constellation Sagittarius

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Chi<sup>1</sup> Sagittarii Star in the constellation Sagittarius

Chi1 Sagittarii (χ1 Sagittarii) is a binary star system in the zodiac constellation of Sagittarius. The pair have a combined apparent visual magnitude of +5.03, which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 12.95 mas as seen from Earth, it is located around 252 light years from the Sun. It is advancing through space in the general direction of the Earth with a radial velocity of −43.4 km/s.

Kappa<sup>1</sup> Sagittarii Star in the constellation Sagittarius

Kappa1 Sagittarii (κ1 Sagittarii) is a solitary, white-hued star in the zodiac constellation of Sagittarius. It has an apparent visual magnitude of +5.58, which is bright enough to be faintly visible to the naked eye. According to the Bortle scale, it can be viewed from dark suburban skies. Based upon an annual parallax shift of 15.12 mas as seen from Earth, this star is located around 223 light years from the Sun. It is advancing in the general direction of the Sun with a radial velocity of −11.6 km/s.

KW Sagittarii is a red supergiant, located approximately 1,900 parsecs away from the Sun in the direction of the constellation Sagittarius. It is one of the largest-known stars. If placed at the center of the Solar System, the star's surface would engulf Mars.

<span class="mw-page-title-main">V4641 Sagittarii</span> Binary star in the constellation Sagittarius

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VX Sagittarii is an extreme 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 also one of the largest stars discovered so far, 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 au). It is the most luminous known AGB star, at bolometric magnitude –8.6, which is even brighter than the theoretical limit at –8.0.

<span class="mw-page-title-main">7 Sagittarii</span> Star in the constellation Sagittarius

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56 Sagittarii is a single star in the southern constellation of Sagittarius. It has the Bayer designation f Sagittarii, while 56 Sagittarii is the Flamsteed designation. This object is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.87. It is located approximately 208 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +22 km/s.

<span class="mw-page-title-main">U Sagittarii</span> Star in the constellation Sagittarius

U Sagittarii is a variable star in the southern constellation of Sagittarius, abbreviated U Sgr. It is a classical Cepheid variable that ranges in brightness from an apparent visual magnitude of 6.28 down to 7.15, with a pulsation period of 6.745226 days. At its brightest, this star is dimly visible to the naked eye. The distance to this star is approximately 2,080 light years based on parallax measurements, and it is drifting further away with a radial velocity of 2 km/s.

<span class="mw-page-title-main">RS Sagittarii</span> Eclipsing binary star system in the constellation Sagittarius

RS Sagittarii is an eclipsing binary star system in the southern constellation of Sagittarius, abbreviated RS Sgr. It is a double-lined spectroscopic binary with an orbital period of 2.416 days, indicating that the components are too close to each other to be individually resolved. The system has a combined apparent visual magnitude of 6.01, which is bright enough to be faintly visible to the naked eye. During the primary eclipse the brightness drops to magnitude 6.97, while the secondary eclipse is of magnitude 6.28. The distance to this system is approximately 1,420 light years based on parallax measurements.

References

  1. 1 2 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, arXiv: 1412.7822 , Bibcode:2015A&A...578A..75T, doi:10.1051/0004-6361/201425592, S2CID   54789582, A75.
  2. 1 2 3 4 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, arXiv: astro-ph/9905016 , Bibcode:1999AJ....118.1034M, doi:10.1086/300951, S2CID   13862209.
  3. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  4. ↑ Kimeswenger, S. (January 2006), "V4332 Sgr in 'Quiescence'", Astronomische Nachrichten, 327 (1): 44–52, arXiv: astro-ph/0509844 , Bibcode:2006AN....327...44K, doi:10.1002/asna.200510482, S2CID   118936262.
  5. ↑ Özdönmez, Aykut; et al. (September 2016), "The distances of the Galactic novae", Monthly Notices of the Royal Astronomical Society, 461 (2): 1177–1201, arXiv: 1606.01907 , Bibcode:2016MNRAS.461.1177O, doi:10.1093/mnras/stw1362.
  6. ↑ "V4332 Sgr". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2022-02-05.{{cite web}}: CS1 maint: postscript (link)
  7. ↑ Hayashi, S. S.; et al. (February 1994), Marsden, B. G. (ed.), "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. 1 2 3 Tylenda, R.; et al. (August 2005), "V4332 Sagittarii revisited", Astronomy and Astrophysics, 439 (2): 651–661, arXiv: astro-ph/0412205 , Bibcode:2005A&A...439..651T, doi:10.1051/0004-6361:20041581, S2CID   119410176.
  10. ↑ Soker, Noam; Tylenda, Romuald (January 2003), "Main-Sequence Stellar Eruption Model for V838 Monocerotis", The Astrophysical Journal, 582 (2): L105–L108, arXiv: astro-ph/0210463 , Bibcode:2003ApJ...582L.105S, doi:10.1086/367759, S2CID   18351411.
  11. ↑ Banerjee, Dipankar. P. K.; et al. (December 2015), "Evolution of the Dust in V4332 Sagittarii", The Astrophysical Journal, 814 (2): 9, arXiv: 1510.05074 , Bibcode:2015ApJ...814..109B, doi:10.1088/0004-637X/814/2/109, S2CID   119299700, 109.{{citation}}: CS1 maint: multiple names: authors list (link)

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