V669 Cassiopeiae

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V669 Cassiopeiae
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Cassiopeia
Right ascension 01h 33m 51.21s [1]
Declination 62° 26′ 53.2″ [1]
Apparent magnitude  (V)17.48 [2]
Characteristics
Evolutionary stage AGB [3]
Spectral type M9III [3]
Apparent magnitude  (J)16.747 [1]
Apparent magnitude  (H)11.232 [1]
Apparent magnitude  (K)7.097 [1]
Variable type Mira? [4]
Astrometry
Proper motion (μ)RA: −2.813 [5]   mas/yr
Dec.: −2.147 [5]   mas/yr
Parallax (π)1.9523 ± 0.7049  mas [5]
Distance 2,100 [6]   pc
Details
Radius 370 –702 [6]   R☉
Luminosity 10,000 - 36,000 [6]   L☉
Temperature 3,000 [6]   K
Database references
SIMBAD data

V669 Cassiopeiae or V669 Cas is an OH/IR star, a type of particularly cool red giant, with a spectral type of M9III.

With a mean visual apparent magnitude 17.5, V669 Cassiopeiae varies with an amplitude of about half a magnitude. [2] In the mid-infrared L band, its magnitude range is 1.57 to 3.02. It is listed as a possible Mira variable, but with the extremely long period of 1,994 days. [4]

Jan Herman and Harm Jan Habing reported in 1985 that the star's OH maser emission varied in intensity with a 1994 day period. [7] In 1990, Paolo Persi et al. showed that V669 Cassiopeiae varied in infrared brightness, [8] and for that reason it was given its variable star designation in 1993. [9]

The distance and physical properties of V669 Cassiopeiae are highly uncertain. Based on parallax, it is about 1,600 light years away, but a distance of about 20,000 light years has been derived based on observations of masers around the star. [3] Based on a luminosity derived from its pulsations and spectral energy distribution, it would be at a distance of 6,850 light years. [6]

See also

Related Research Articles

<span class="mw-page-title-main">Mira variable</span> Type of variable star

Mira variables are a class of pulsating stars characterized by very red colours, pulsation periods longer than 100 days, and amplitudes greater than one magnitude in infrared and 2.5 magnitude at visual wavelengths. They are red giants in the very late stages of stellar evolution, on the asymptotic giant branch (AGB), that will expel their outer envelopes as planetary nebulae and become white dwarfs within a few million years.

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

Omicron Cassiopeiae is a triple star system in the constellation Cassiopeia. It is approximately 700 light-years from Earth, based on its parallax. It is visible to the naked eye with a slightly variable apparent magnitude of about 4.5.

<span class="mw-page-title-main">4 Cassiopeiae</span> Star in the constellation Cassiopeia

4 Cassiopeiae is a red giant in the northern constellation of Cassiopeia, located approximately 790 light-years away from the Sun. It is visible to the naked eye as a faint, red-hued star with a baseline apparent visual magnitude of 4.96. At the distance of this system, its visual magnitude is diminished by an extinction of 0.56 due to interstellar dust. This system is moving closer to the Earth with a heliocentric radial velocity of −39 km/s.

<span class="mw-page-title-main">R Centauri</span> Variable star in the constellation Centaurus

R Centauri is a Mira variable star in the constellation Centaurus.

<span class="mw-page-title-main">T Cephei</span> Star in the constellation Cepheus

T Cephei is a Mira variable star in the constellation Cepheus. Located approximately 600 light-years distant, it varies between magnitudes 5.2 and 11.3 over a period of around 388 days.

<span class="mw-page-title-main">S Persei</span> Red supergiant or hypergiant variable star in the constellation Perseus

S Persei is a red supergiant or hypergiant located near the Double Cluster in Perseus, north of the cluster NGC 869. It is a member of the Perseus OB1 association and one of the largest known stars. If placed in the Solar System, its photosphere would engulf the orbit of Jupiter. It is also a semiregular variable, a star whose variations are less regular than those of Mira variables.

<span class="mw-page-title-main">TX Camelopardalis</span> Star in the constellation Camelopardalis

TX Camelopardalis is a Mira-type variable star in the constellation Camelopardalis. It is a classical long period variable star with pulsational period of 558.7 days. Water masers have been observed around the star.

<span class="mw-page-title-main">VX Sagittarii</span> Asymptotic giant branch star in the constellation Sagittarius

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 au). It is the most luminous known AGB star, at bolometric magnitude –8.6, which is brighter than the theoretical limit at –8.0.

<span class="mw-page-title-main">W Hydrae</span> Variable star in the constellation Hydra

W Hydrae is a Mira-type variable star in the constellation Hydra. The star is nearly located within the Solar neighborhood, between 75 and 120 parsecs, likely at 320 light years from the Sun. It has a visual apparent magnitude range of 5.6 to 10. In the near-infrared J band it has a magnitude of -1.7, is the 7th brightest star in the night sky, and is even brighter than Sirius.

<span class="mw-page-title-main">OH/IR star</span>

An OH/IR star is an asymptotic giant branch (AGB) or a red supergiant or hypergiant star that shows strong OH maser emission and is unusually bright at near-infrared wavelengths.

<span class="mw-page-title-main">PZ Cassiopeiae</span> Star in the constellation Cassiopeia

PZ Cassiopeiae is a red supergiant star located in the constellation of Cassiopeia, and a semi-regular variable star.

<span class="mw-page-title-main">Y Centauri</span> Variable star in the constellation Centaurus

Y Centauri or Y Cen is a semiregular variable star in the constellation of Centaurus.

<span class="mw-page-title-main">W Aquilae</span> Variable star in the constellation Aquila

W Aquilae is a variable star in the constellation of Aquila. It is a type of evolved star known as an S-type star. Due to its relatively close distance of 1,200 light-years and equatorial location, it is easy to observe and heavily studied.

<span class="mw-page-title-main">S Cassiopeiae</span> Star in the constellation Cassiopeia

S Cassiopeiae is a Mira variable and S-type star in the constellation Cassiopeia. It is an unusually cool star, rapidly losing mass and surrounded by dense gas and dust producing masers.

<span class="mw-page-title-main">IK Tauri</span> Mira variable star in the constellation Taurus

IK Tauri or NML Tauri is a Mira variable star located about 280 parsecs (910 ly) from the Sun in the zodiac constellation of Taurus.

<span class="mw-page-title-main">II Lupi</span> Star in the constellation Lupus

II Lupi is a Mira variable and carbon star located in the constellation Lupus. It is the brightest carbon star in the southern hemisphere at 12 μm.

<span class="mw-page-title-main">QV Andromedae</span> Star in the constellation Andromeda

QV Andromedae is an Alpha2 Canum Venaticorum variable in the constellation Andromeda. Its maximum apparent visual magnitude is 6.6, so it can be seen by the naked eye under very favourable conditions. The brightness varies slightly following a periodic cycle of approximately 5.23 days.

<span class="mw-page-title-main">EP Aquarii</span> Variable star in the constellation Aquarius

EP Aquarii is a semiregular variable star in the equatorial constellation of Aquarius. At its peak brightness, visual magnitude 6.37, it might be faintly visible to the unaided eye under ideal observing conditions. A cool red giant on the asymptotic giant branch (AGB), its visible light brightness varies by about 1/2 magnitude over a period of 55 days. EP Aquarii has a complex circumstellar envelope (CSE), which has been the subject of numerous studies.

<span class="mw-page-title-main">RT Virginis</span> Star in the constellation Virgo

RT Virginis is a variable star in the equatorial constellation of Virgo, abbreviated RT Vir. It ranges in brightness from an apparent visual magnitude of 7.7 down to 9.7, which is too faint to be visible to the naked eye. Based on parallax measurements made with the VLBI, the distance to this star is approximately 740 light years. It is receding from the Sun with a radial velocity of 17 km/s.

<span class="mw-page-title-main">R Crateris</span> Variable star in the constellation Crater

R Crateris is a star about 700 light years from the Earth in the constellation Crater. It is a semiregular variable star, ranging in brightness from magnitude 8.1 to 9.5 over a period of about 160 days. It is not visible to the naked-eye, but can be seen with a small telescope, or binoculars. R Crateris is a double star; the variable star and its magnitude 9.9 F8V companion are separated by 65.4 arcseconds.

References

  1. 1 2 3 4 5 Cutri, Roc M.; et al. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  2. 1 2 Jayasinghe, T.; Kochanek, C. S.; Stanek, K. Z.; Shappee, B. J.; Holoien, T. W. -S.; Thompson, Todd A.; Prieto, J. L.; Dong, Subo; Pawlak, M.; Shields, J. V.; Pojmanski, G.; Otero, S.; Britt, C. A.; Will, D. (2018). "The ASAS-SN catalogue of variable stars I: The Serendipitous Survey". Monthly Notices of the Royal Astronomical Society. 477 (3): 3145. arXiv: 1803.01001 . Bibcode:2018MNRAS.477.3145J. doi: 10.1093/mnras/sty838 .
  3. 1 2 3 De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae". Astronomy and Astrophysics. 523: A18. arXiv: 1008.1083 . Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771. S2CID   16131273.
  4. 1 2 Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports . 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID   125853869.
  5. 1 2 3 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  6. 1 2 3 4 5 Lombaert, R.; Decin, L.; De Koter, A.; Blommaert, J. A. D. L.; Royer, P.; De Beck, E.; De Vries, B. L.; Khouri, T.; Min, M. (2013). "H2O vapor excitation in dusty AGB envelopes. A PACS view of OH 127.8+0.0". Astronomy and Astrophysics. 554. arXiv: 1505.07696 . Bibcode:2013A&A...554A.142L. doi:10.1051/0004-6361/201218974. S2CID   98319654.
  7. ↑ Herman, J.; Habing, H. J. (March 1985). "Time variations and shell sizes of OH masers in late-type stars". Astronomy and Astrophysics, Supplement Series. 59: 523–555. Bibcode:1985A&AS...59..523H . Retrieved 29 August 2024.
  8. ↑ Persi, P.; Ferrari-Toniolo, M.; Shivanandan, K.; Ranieri, M.; Marenzi, A. (October 1990). "Infrared photometry up to 34 mu.m of the type II OH/IR sources OH 127.8-0.0 and OH 345.0+15.7". Astronomy and Astrophysics. 237: 153–158. Bibcode:1990A&A...237..153P . Retrieved 29 August 2024.
  9. ↑ Kazarovets, E. V.; Samus, N. N.; Goranskij, V. P. (February 1993). "The 71st Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 3840 (3840): 1. Bibcode:1993IBVS.3840....1K . Retrieved 29 August 2024.
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