V603 Aquilae
| 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]
First seen by Zygmunt Laskowski, a medical professor and amateur astronomer,[3] and then confirmed on the night of 8 June 1918 by the professional astronomer Grace Cook,[4] 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.[5] Tycho's and Kepler's supernovae were brighter, but both occurred before the invention of the telescope.[6] 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[when?] determined to be true for several other novae at the time.[7]
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.[8] This second star is most likely a red dwarf.[1] The two stars orbit each other approximately every 3 hours 20 minutes.[8]
References
- ↑ 1.0 1.1 1.2 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 2.0 2.1 2.2 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ The Contribution of Amateurs to Astronomy, Proceedings of Colloquium 98 of the International Astronomical Union, June 20–24, 1987, page 41
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 8.0 8.1 Lua error in package.lua at line 80: module 'strict' not found.
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- Image V603 Aquilae
