V603 Aquilae

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V603 Aquilae or Nova Aquilae 1918
Observation data
Epoch J2000      Equinox J2000
Constellation Aquila
Right ascension 18h 48m 54.6366s
Declination +00° 35′ 02.863″
Apparent magnitude (V) 11.64
Characteristics
Spectral type sd:Be+
B−V color index -0.2 ± 0.5
Variable type Variable star
Astrometry
Radial velocity (Rv) -23 km/s
Proper motion (μ) RA: 10.81 mas/yr
Dec.: -8.86 mas/yr
Parallax (π) 4.21 ± 2.59 mas
Distance approx. 800 ly
(approx. 200 pc)
Absolute magnitude (MV) 11.65
Details
Radius 0,72 R
Luminosity -0,14594 L
Temperature 145 K
Other designations
Nova Aql 1918, Nova Aquilae 1918, EM* CDS 1028, HD 174107, 1RXS J184854.7+003501, ALS 9992, 1ES 1846+00.5, SBC7 706, AN 7.1918, FASTT 1189, HIP 92316, UBV M 51004, CSI+00-18463, GCRV 68659, KPD 1846+0031, 2E 1846.3+0031, LS IV +00 3, 2E 4138, GSC 00448-00423, 2MASS J18485464+0035030, EM* RJHA 116, HBHA 202-05, PLX 4341, AAVSO 1843+00.
Database references
SIMBAD data
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

V603 Aquilae (or Nova Aquilae 1918) was a bright nova occurring in the constellation Aquila in 1918. It is a binary system, comprising a white dwarf and donor low-mass star in close orbit to the point of being only semidetached. The white dwarf sucks matter off its companion, which has filled its Roche lobe,[1] onto its accretion disk and surface until the excess material is blown off in a thermonuclear event.[2] This material then forms an expanding shell, which eventually thins out and disappears.[1]

Discovered on the night of 8 June 1918,[3] Nova Aquilae reached a peak magnitude of −0.5; it was the brightest nova recorded in the era of the telescope.[2] It was brighter than all stars bar Sirius and Canopus.[4] Tycho's and Kepler's supernovae were brighter, but both occurred before the invention of the telescope.[5] Originally a star system with a magnitude of 11.43, it took twelve days to fade three magnitudes and then 18.6 years to fade to quiescence.[2] In 1964 Robert P. Kraft ascertained that it was a binary system, recently determined to be true for several other novae at the time.[6]

The star system has settled to an average apparent magnitude of 11.4 since the 1940s, fading by around 1/100th of a magnitude per decade. Spectroscopic analysis conducted by Arenas and colleagues indicated the system consisted of a white dwarf of about 1.2 times as massive as the sun, with an accretion disk, and a companion star with about 20% of the Sun's mass.[7] This second star is most likely a red dwarf.[1] The two stars orbit each other approximately every 3 hours 20 minutes.[7]

References[edit]

  1. ^ a b c Selvelli, P. L.; Cassatella, A.; Cassatella (1981). "Nova AQL 1918 - A nude old nova". In: Effects of mass loss on stellar evolution; Proceedings of the Fifty-ninth Colloquium, Trieste, Italy, September 15–19, 1980. (A82-33926 16-90) Dordrecht, D. Reidel Publishing Co. 89: 515–522. Bibcode:1981ASSL...89..515S. doi:10.1007/978-94-009-8500-1_74. 
  2. ^ a b c Johnson, Christopher B.; Schaefer, Bradley E.; Kroll , Peter; Henden, Arne A. (2013). "Nova Aquilae 1918 (V603 Aql) Faded by 0.44 mag/century from 1938-2013". arXiv:1310.6802. Bibcode:2014ApJ...780L..25J. doi:10.1088/2041-8205/780/2/L25. 
  3. ^ Mobberley, Martin (2009). Cataclysmic Cosmic Events and How to Observe Them. Springer. p. 46. ISBN 038779946X. 
  4. ^ Moore, Patrick (2006). The Amateur Astronomer. Springer. p. 145. ISBN 1846282861. 
  5. ^ Drechsel, H., Holm, A., Krautter, J., & Rahe, J. (1981). "Phase-dependent optical and ultraviolet observations of the old nova V603 Aquilae (1918)". Astronomy & Astrophysics 99 (1): 166–72. Bibcode:1981A&A....99..166D. 
  6. ^ Kraft, Robert P. (1964). "Binary stars among cataclysmic variables. III. Ten old novae". Astrophysical Journal 139: 457–75. Bibcode:1964ApJ...139..457K. doi:10.1086/147776. 
  7. ^ a b Arenas, J.; Catalán, M. S.; Augusteijn, T.; Retter, A. "A spectroscopic study of V603 Aquilae: stellar parameters and continuum-line variations". Monthly Notices of the Royal Astronomical Society 311 (1): 135–48. Bibcode:2000MNRAS.311..135A. doi:10.1046/j.1365-8711.2000.03061.x. 

External links[edit]