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Henry Draper Catalogue objectsNovaeAquila (constellation)Astronomical objects discovered in 1918Objects with variable star designationsHipparcos objects
novaAquilaRoche lobeaccretion diskGrace CookmagnitudeSiriusCanopusTycho'sKepler'sRobert P. Kraftwhite dwarfred dwarf
| 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 |
| Distance | 810+29 −26 ly (7002249000000000000♠249+9 −8[1] pc) |
| Absolute magnitude (MV) | 11.65 |
| 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 |
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,[2] onto its accretion disk and surface until the excess material is blown off in a thermonuclear event.[3] This material then forms an expanding shell, which eventually thins out and disappears.[2]
First seen by Zygmunt Laskowski, a medical professor and amateur astronomer,[4] and then confirmed on the night of 8 June 1918 by the UK amateur astronomer Grace Cook,[5] Nova Aquilae reached a peak magnitude of −0.5; it was the brightest nova recorded in the era of the telescope.[3] It was brighter than all stars but Sirius and Canopus.[6]Tycho's and Kepler's supernovae were brighter, but both occurred before the invention of the telescope.[7] 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.[3] In 1964 Robert P. Kraft ascertained that it was a binary system, recently[when?] determined to be true for several other novae at the time.[8]
The star system has settled to an average apparent magnitude of 11.4 since the 1940s, fading by around 1/100 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.[9] This second star is most likely a red dwarf.[2] The two stars orbit each other approximately every 3 hours 20 minutes.[9]
References
^ Harrison, Thomas E.; et al. (2013). "Hubble Space Telescope Fine Guidance Sensor Parallaxes for Four Classical Novae". The Astrophysical Journal. 767 (1). 7. arXiv:1302.3245. Bibcode:2013ApJ...767....7H. doi:10.1088/0004-637X/767/1/7..mw-parser-output cite.citation{font-style:inherit}.mw-parser-output .citation q{quotes:"""""""'""'"}.mw-parser-output .citation .cs1-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .citation .cs1-lock-limited a,.mw-parser-output .citation .cs1-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .citation .cs1-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration{color:#555}.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration span{border-bottom:1px dotted;cursor:help}.mw-parser-output .cs1-ws-icon a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/4/4c/Wikisource-logo.svg/12px-Wikisource-logo.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output code.cs1-code{color:inherit;background:inherit;border:inherit;padding:inherit}.mw-parser-output .cs1-hidden-error{display:none;font-size:100%}.mw-parser-output .cs1-visible-error{font-size:100%}.mw-parser-output .cs1-maint{display:none;color:#33aa33;margin-left:0.3em}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-format{font-size:95%}.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-right{padding-right:0.2em}
^ abc Selvelli, P. L.; Cassatella, A. (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. Astrophysics and Space Science Library. 89: 515–522. Bibcode:1981ASSL...89..515S. doi:10.1007/978-94-009-8500-1_74. ISBN 978-94-009-8502-5.
^ abc 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". The Astrophysical Journal. 780 (2): L25. arXiv:1310.6802. Bibcode:2014ApJ...780L..25J. doi:10.1088/2041-8205/780/2/L25.
^ The Contribution of Amateurs to Astronomy, Proceedings of Colloquium 98 of the International Astronomical Union, June 20–24, 1987, page 41
^ Mobberley, Martin (2009). Cataclysmic Cosmic Events and How to Observe Them. Springer. p. 46. ISBN 978-0387799469.
^ Moore, Patrick (2006). The Amateur Astronomer. Springer. p. 145. ISBN 978-1846282867.
^ 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.
^ 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.
^ ab Arenas, J.; Catalán, M. S.; Augusteijn, T.; Retter, A. (2000). "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.
Pottasch, Stuart (1959). "The nova outburst: V. The temperature and radius of the central exciting star and observation". SAO/NASA Astrophysics Data System (ADS). 22: 416. Bibcode:1959AnAp...22..412P.
- Image V603 Aquilae
External links
- www.otticademaria.it
- HIC 92316
- HIP 92316
