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DX Andromedae

DX Andromedae

The visual band light curve of DX Andromedae, from AAVSO data, showing three eruptions[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension 23h 29m 46.6839s[2]
Declination +43° 45′ 04.03439″[2]
Apparent magnitude (V) 11.0 – 15.5 variable [3]
Characteristics
Spectral type pec(UG)[3] (K1 V[4])
Apparent magnitude (B) 11.00[5]
Apparent magnitude (G) 14.7821[2]
Apparent magnitude (J) 13.106[6]
Apparent magnitude (H) 12.512[6]
Apparent magnitude (K) 12.390[6]
Variable type Dwarf nova
Astrometry
Radial velocity (Rv)-2[5] km/s
Proper motion (μ) RA: −8.343±0.035[2] mas/yr
Dec.: −9.835±0.030[2] mas/yr
Parallax (π)1.6685 ± 0.0249 mas[2]
Distance1,950 ± 30 ly
(599 ± 9 pc)
Orbit
Period (P)10.6 hours[7]
Inclination (i)45[8]°
Details[8]
White Dwarf
Mass0.8 (assumed) M☉
Temperature25,000 K
Donor star
Surface gravity (log g)4.0 cgs
Temperature5,000 K
Metallicity [Fe/H]0 dex
Rotational velocity (v sin i)79±5 km/s
Other designations
2MASS J23294667+4345040
Database references
SIMBADdata

DX Andromedae (often abbreviated to DX And) is a cataclysmic variable star in the constellation Andromeda. It has a typical apparent visual magnitude of 15.5 during the quiescent phase, but becomes brighter (up to a magnitude of 11.0) during outbursts recurring with a mean cycle length of 330 days,[7] thus is classified as a dwarf nova of the SS Cygni type.[3]

System

The system of DX Andromedae consists of a white dwarf accreting matter from a donor star through an accretion disk. The system shows a spectral type at quiescence of K1 V (plus emission lines),[4] but the donor is considered to be a hydrogen-deficient star that has evolved off the main sequence and is overfilling its roche lobe. The donor star dominates the visible spectrum during the quiescent phase.[7][8]

The spectral classification of DX Andromedae as a whole is classified as peculiar of the U Geminorum type.[3] The spectrum of the donor star is itself peculiar; enhanced absorption lines of CaI and CrI have been observed.[4]

Variability

DX Andromedae was discovered by Giuliano Romano on a series of photographic plates begun on September 28, 1956. Its discovery was announced in 1958.[9]

The outburst of dwarf novae are thought to arise from a thermal instability of the disk, that increases mass flow and temperature and hence the luminosity increases. In DX Andromedae different outbursts don't reach the same peak luminosity and don't occur at a regular rate, but they retain the same shape in the decaying part. It seems that the peak luminosity is correlated to the length of the preceding cycle, and the more luminous is the outburst, the faster the luminosity peak is reached. These trends can be explained by matter accumulating in the disk; more matter is accumulated in the disk during a longer cycle, and it can power a stronger outburst.[7]

References

  1. ^ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  2. ^ a b c d e f 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.
  3. ^ a b c d DX 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. ^ a b c Bruch, A.; Vrielmann, S.; Hessman, F. V.; Kochsiek, A.; Schimpke, T. (November 1997). "A spectroscopic study of the long-period dwarf nova DX Andromedae". Astronomy and Astrophysics. 327: 1107–1113. Bibcode:1997A&A...327.1107B.
  5. ^ a b "DX And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved November 1, 2018.
  6. ^ 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.
  7. ^ a b c d Šimon, V. (2000). "Activity of DX Andromedae - the dwarf nova with a very long recurrence time of outbursts". Astronomy and Astrophysics. 364: 694–700. Bibcode:2000A&A...364..694S.
  8. ^ a b c Harrison, T. E. (2018), "The Identification of Hydrogen-deficient Cataclysmic Variable Donor Stars", The Astrophysical Journal, 861 (2): 102, arXiv:1806.04612, Bibcode:2018ApJ...861..102H, doi:10.3847/1538-4357/aacbd9, S2CID 119531169.
  9. ^ Romano, G. (1958). "La nuova variabile del tipo U Geminorum". Memorie della Società Astronomia Italiana. 29: 177. Bibcode:1958MmSAI..29..177R. Retrieved 30 October 2024.
Quelle: https://en.wikipedia.org/wiki/DX_Andromedae