AR Andromedae

AR Andromedae

A visual band light curve for AR Andromedae, from AAVSO data, showing five outbursts.[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension 01h 45m 03.27155s[2]
Declination +37° 58′ 33.2379″[2]
Apparent magnitude (V) 11.0 – 17.6 variable[3]
Characteristics
Spectral type pec(UG)[3]
Apparent magnitude (B) 12.8
Apparent magnitude (V) 11.00[4]
Apparent magnitude (G) 16.3185[2]
Apparent magnitude (J) 14.589[5]
Apparent magnitude (H) 13.996[5]
Apparent magnitude (K) 13.730[5]
Variable type UGSS[3]
Astrometry
Proper motion (μ) RA: 5.431±0.046[2] mas/yr
Dec.: −7.249±0.059[2] mas/yr
Parallax (π)2.4070 ± 0.0666 mas[2]
Distance1,360 ± 40 ly
(420 ± 10 pc)
Orbit[6]
Period (P)0.16302±0.00032 days
Periastron epoch (T)HJD 2450005.6924±0.0021
Semi-amplitude (K1)
(primary)		91±7 km/s
Other designations
2MASS J01450327+3756334, CRTS J014503.3+375633[7]
Database references
SIMBADdata

AR Andromedae (AR And) is a dwarf nova of the SS Cygni type in the constellation Andromeda. Its typical apparent visual magnitude is 17.6, but increases up to 11.0 magnitude during outbursts. The outbursts occur approximately every 23 days.[3]

System

[edit]

Dwarf novae systems are made up by a classical star with a white dwarf companion. By measuring the Doppler shift of spectral lines, it was found to have an orbital period of 3.91 hours.[6] The accretion disk around white dwarf seems to be axisymmetric and devoid of structure.[8]

Variability

[edit]

AR Andromedae was first listed as a variable star by Frank Elmore Ross in 1929, based on observations in 1907 (when the star was too faint to detect) and 1927 (when the star had flared to magnitude 12).[9] It was initially classified as a Mira variable star.[10] In 1934 it was given the variable star designation AR Andromedae.[11]

The light emitted by dwarf novae like AR Andromedae comes entirely from the accretion disc and the white dwarf; the luminosity increase during outbursts is typically induced by a variation in the accretion rate of the white dwarf. The outbursts are unusually frequent, with 19 outbursts detected by 2016.[12]

Spectrum

[edit]

The spectral type of AR Andromedae is classified as peculiar of the U Geminorum type,[3] since the spectrum is not a typical stellar blackbody. It also shows strong emission lines of the first two Balmer series lines as well as HeI ones. In addition, an unusually strong FeII line with other possible weak lines of the same origin were also reported.[6]

References

[edit]
  1. ^ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  2. ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. ^ a b c d e AR 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 2018-10-24.
  4. ^ Database entry, Catalogue of Stellar Photometry in Johnson's 11-color system (2002 Ed.), J. R. Ducati, CDS ID [1] Accessed on line 2018-10-24.
  5. ^ a b c 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. ^ a b c Taylor, C. J.; Thorstensen, J. R. (October 1996). "Orbital Periods of the Dwarf Novae AR And, AM Cas, and PY Per". Publications of the Astronomical Society of the Pacific. 108: 894. Bibcode:1996PASP..108..894T. doi:10.1086/133810.
  7. ^ "AR And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved October 24, 2018.
  8. ^ Ruiz-Carmona, R.; Groot, P. J.; Steeghs, D. (2019), "A systematic study of spiral density waves in the accretion discs of cataclysmic variables", Monthly Notices of the Royal Astronomical Society, 491 (2): 2217–2253, arXiv:1910.12089, doi:10.1093/mnras/stz2992
  9. ^ Ross, F. E. (August 1929). "New variable stars (eight list) - New proper-motion stars. (seventh list)". Astronomical Journal. 39: 140–142. Bibcode:1929AJ.....39..140R. doi:10.1086/104923. Retrieved 12 March 2023.
  10. ^ Morgenroth, O. (December 1933). "62 neue Veränderlilche". Astronomische Nachrichten. 250 (5): 75. Bibcode:1933AN....250...75M. doi:10.1002/asna.19332500503. Retrieved 12 March 2023.
  11. ^ Guthnick, P.; Prager, R. (April 1934). "Benennung von veränderlichen Sternen". Astronomische Nachrichten. 251 (17): 257. Bibcode:1934AN....251..257G. doi:10.1002/asna.19342511702. Retrieved 12 March 2023.
  12. ^ Statistical properties of dwarf novae-type cataclysmic variables: the outburst catalogue supplementary data
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