QV Andromedae

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QV Andromedae
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 01h 16m 24.4904s [1]
Declination +48° 04′ 56.00453″ [1]
Apparent magnitude  (V)6.608 (variable) [2]
Characteristics
Spectral type B9IIIpSi [3]
Apparent magnitude  (U)6.23 [4]
Apparent magnitude  (B)6.559 [2]
Apparent magnitude  (V)6.608 [2]
Apparent magnitude  (G)6.5628 [1]
Apparent magnitude  (J)6.554 [5]
Apparent magnitude  (H)6.638 [5]
Apparent magnitude  (K)6.657 [5]
U−B color index -0.35 [6]
B−V color index -0.04335 [2]
Variable type ACV
Astrometry
Radial velocity (Rv)−13.6±3 [7]  km/s
Proper motion (μ)RA: 9.696±0.121 [1]   mas/yr
Dec.: 2.699±0.166 [1]   mas/yr
Parallax (π)4.4041 ± 0.0914 [1]   mas
Distance 740 ± 20  ly
(227 ± 5  pc)
Details
Mass 4.4 [8]   M☉
Luminosity 266.63 [9]   L☉
Surface gravity (log g)3.541±0.039 [8]   cgs
Temperature 12384±150 [8]   K
Rotational velocity (v sin i)49±15 [8]  km/s
Other designations
2MASS  J01162450+4804561, BD+47 357, FK5  2085, HD  7546, HIP  5939, HR  369, SAO  37067, TYC  3268-835-1
Database references
SIMBAD data

QV Andromedae (abbreviated to QV And, also known as HR 369 in the Bright Star Catalogue) 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. [3]

The stellar classification of this star is B9IIIpSi, [3] where the pSi suffix indicates that the star shows peculiar chemical composition with stronger than usual silicon lines. This type of star is known as an Ap star, with the chemical peculiarities caused by strong magnetic fields and slow rotation leading to chemical stratification in the atmosphere. [6] The star is rotating at a projected rotational velocity of 49 km/s, [8] with up to 0.05 magnitude variation of brightness during one rotation cycle. This leads to the classification of the star as an Alpha2 Canum Venaticorum variable. [3]

The variability of QV Andromedae was first identified in 1975, [10] and confirmed from Hipparcos photometry. [11] It was assigned the variable star designation QV Andromedae in the 73rd namelist of variable stars in 1997. [12]

Related Research Articles

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Chi Serpentis is a solitary star in the Serpens Caput section of the equatorial constellation Serpens. Based upon an annual parallax shift of 14.84 mas as seen from Earth, it is located around 220 light years from the Sun. The star is bright enough to be faintly visible to the naked eye, having an apparent visual magnitude of +5.30.

Zeta Andromedae is a star system in the constellation Andromeda. It is approximately 189 light-years from Earth.

63 Andromedae is an Alpha2 Canum Venaticorum variable star in the constellation Andromeda. Its variable star designation is PZ Andromedae. With an apparent magnitude of about 5.6, it is bright enough to be seen by naked eye. Based upon an annual parallax shift of 7.8991 mas, it is located 413 light years away.

13 Andromedae Star in the constellation Andromeda

13 Andromedae, abbreviated 13 And, is a single, blue-white hued variable star in the northern constellation of Andromeda. 13 Andromedae is the Flamsteed designation, while it bears the variable star designation V388 Andromedae. With a typical apparent visual magnitude of around 5.75, it is dimly visible to the naked eye under good seeing conditions. The distance to this star can be directly estimated from its annual parallax shift of 10.9 mas, yielding a range of 300 light years. At that distance, its brightness is diminished by an extinction of 0.13 magnitude due to interstellar dust. The star is moving closer to the Earth with a heliocentric radial velocity of −8 km/s.

53 Camelopardalis is a binary star system in the northern circumpolar constellation of Camelopardalis, located 290 light years away from the Sun as determined by parallax measurements. It has the variable star designation AX Camelopardalis; 53 Camelopardalis is the Flamsteed designation. This object is dimly visible to the naked eye as a white hued star with a baseline apparent visual magnitude of +6.02. It is a single-lined spectroscopic binary system with an orbital period of 6.63 years and a high eccentricity of 0.718. The "a sin i" value of the primary is 280 Gm (1.9 AU), where a is the semimajor axis and i is the orbital inclination.

20 Canum Venaticorum is a single variable star in the northern constellation of Canes Venatici, located 238 light years from the Sun. This object has the variable star designation AO Canum Venaticorum; 20 Canum Venaticorum is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a baseline apparent visual magnitude of +4.72. The star is moving further from the Earth with a heliocentric radial velocity of +9 km/s. Eggen (1971) listed this star as a member of the Hyades Stream.

21 Canum Venaticorum is a single variable star in the northern constellation of Canes Venatici, located 277 light years away from the Sun. This object has the variable star designation BK Canum Venaticorum; 21 Canum Venaticorum is the Flamsteed designation. It is visible to the naked eye as a faint white-hued star with a baseline apparent visual magnitude of +5.14.

4 Canum Venaticorum is a binary star system in the northern constellation of Canes Venatici, located around 425 light years away. It has the variable star designation AI Canum Venaticorum; 4 Canum Venaticorum is its Flamsteed designation. Its brightness varies from magnitude +5.89 to +6.15 with a period of 2.8 hours, which places it around the lower limit of visibility to the naked eye. This was found to be a binary by Schmid et al. in 2014, based on periodic, non-sinusoidal changes in its radial velocity. It is a single-lined spectroscopic binary with an orbital period of 124.4 days and an eccentricity of 0.31.

KK Andromedae Variable star in the constellation Andromeda

KK Andromedae, also known as HD 9531, is a variable star in the northern constellation of Andromeda. It has an apparent visual magnitude of 5.90, which places it near the lower limit of visibility to the naked eye even under good viewing conditions. An Alpha2 Canum Venaticorum variable, it varies in brightness by 0.012 magnitude every 0.66 days. Based upon an annual parallax shift of 7.5 mas as seen from Earth, it is located around 437 light years from the Sun. At that distance, the brightness of the star is diminished by an extinction of 0.26 magnitude due to interstellar dust.

HD 4778, also known as HR 234 and GO Andromedae, is a variable star in the constellation Andromeda. Its magnitude varies by 0.04 magnitudes from the median of 6.12 with a period of approximately 2.55 days. The star is located 350 light years away, as determined from its annual parallax shift of 9.32 mas.

HD 224801, also known as CG Andromedae, is an Alpha² Canum Venaticorum variable star in the constellation Andromeda. Located approximately 188 parsecs (610 ly) away, the star varies between apparent magnitudes 6.32 and 6.42 over a period of approximately 3.74 days.

ET Andromedae Star in the constellation Andromeda

ET Andromedae is a binary star system star in the northern constellation of Andromeda. It has an apparent visual magnitude of 6.48, placing it at the nominal limit for visibility with the naked eye. The distance to this system can be estimated from its annual parallax shift of 5.42 mas, which yields a value of 602 light years.

VZ Arietis is single, white-hued star in the northern zodiac constellation of Aries. Varying between magnitudes 5.82 and 5.89, the star can be seen with the naked eye in dark, unpolluted areas. Based upon an annual parallax shift of 5.8 mas, it is located 560 light years from the Sun. It is moving further away with a heliocentric radial velocity of +14 km/s. The star was formerly known as 16 Trianguli, but as the star is no longer in the constellation Triangulum, this designation has fallen out of use.

IQ Aurigae Single, variable star in the constellation Auriga

IQ Aurigae is a single, variable star in the northern constellation of Auriga. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude that fluctuates around 5.38. The star is located at a distance of about 470 light-years from the Sun based on parallax and is drifting further away with a radial velocity of +28.6 km/s.

BX Boötis A type main sequence star in the constellation Boötes

BX Boötis is a star in the northern constellation of Boötes. It is a dim star near the lower limit of visibility to the naked eye, having a nominal apparent visual magnitude of 6.35. Based upon an annual parallax shift of 10.81 mas, it is located 302 light years away. At that distance, the visual magnitude of the star is diminished by an extinction of 0.13 due to interstellar dust. It is moving closer with a heliocentric radial velocity of −11 km/s.

RT Andromedae Star in the constellation Andromeda

RT Andromedae is a variable star in the constellation of Andromeda. The system is estimated to be 322 light-years away.

HD 3322 is a binary star system in the northern constellation of Andromeda. With an apparent visual magnitude of 6.51, it lies below the nominal brightness limit for visibility with the normal naked eye, but it is still possible to see the star with excellent vision under ideal seeing conditions. An annual parallax shift of 4.59±0.65 mas provides a distance estimate of roughly 700 light years.

GR Andromedae Star in the constellation Andromeda

GR Andromedae is a variable star in the constellation Andromeda. Its apparent visual magnitude varies between 6.87 and 6.95 in a cycle of 518.2 days. It is classified as an α2 Canum Venaticorum variable.

HN Andromedae Star in the constellation Andromeda

HN Andromedae is a variable star in the constellation Andromeda. Its apparent visual magnitude varies between 6.67 and 6.76 in a cycle of 69.51 days. It is classified as an α2 Canum Venaticorum variable.

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 3 4 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy & Astrophysics, 355: L27–L30, Bibcode:2000A&A...355L..27H.
  3. 1 2 3 4 QV And, database entry, Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.), N. N. Samus, O. V. Durlevich, et al., CDS ID II/250 Accessed on line 2018-10-17.
  4. ↑ "QV And". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved October 17, 2018.
  5. 1 2 3 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (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.
  6. 1 2 Renson, P.; Manfroid, J. (2009). "Catalogue of Ap, HgMn and Am stars". Astronomy and Astrophysics. 498 (3): 961–966. Bibcode:2009A&A...498..961R. doi: 10.1051/0004-6361/200810788 .
  7. ↑ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv: 1208.3048 , Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID   59451347, A61.
  8. 1 2 3 4 5 Huang, W.; Gies, D. R.; McSwain, M. V. (2010). "A Stellar Rotation Census of B Stars: From ZAMS to TAMS". The Astrophysical Journal. 722 (1): 605–619. arXiv: 1008.1761 . Bibcode:2010ApJ...722..605H. doi:10.1088/0004-637X/722/1/605. S2CID   118532653.
  9. ↑ McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012). "Fundamental parameters and infrared excesses of Hipparcos stars". Monthly Notices of the Royal Astronomical Society. 427 (1): 343–357. arXiv: 1208.2037 . Bibcode:2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x. S2CID   118665352.
  10. ↑ Winzer, John Ernest (1974). "The Photometric Variability of the Peculiar a Stars". Bibcode:1974PhDT........61W.Cite journal requires |journal= (help)
  11. ↑ Adelman, Saul J. (1998). "On the HIPPARCOS photometry of chemically peculiar B, A, and F stars". Astronomy and Astrophysics Supplement Series. 132: 93–97. Bibcode:1998A&AS..132...93A. doi: 10.1051/aas:1998361 .
  12. ↑ Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V.; Perova, N. B. (1985). "The 67th Name-List of Variable Stars". Information Bulletin on Variable Stars. 2681: 1. Bibcode:1985IBVS.2681....1K.
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