Nova Aquilae 1918

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Double star
Nova Aquilae 1918
AladinLite
Observation
dates equinox :  J2000.0 , epoch : J2000.0
Constellation Eagle
Right ascension 18 h 48 m 54.64 s
declination + 00 ° 35 ′ 2.9 ″
Apparent brightness −0.5 to 11.46 mag
Typing
rel. Brightness
(G-band) 		11.8388 ± 0.0148 mag
rel. Brightness
(J-band) 		11.7 ± 0.026 mag
B − V color index 0.01 
U − B color index −0.92 
Spectral class sdBe
Variable star type N / A 
Astrometry
Radial velocity −25 km / s km / s
parallax (3.1906 ± 0.0686)  mas
distance 810 ± 26  ly
249 ± 8  pc  
Proper movement 
Rec. Share: (11.3 ± 0.141)  mas / a
Dec. portion: (−9.484 ± 0.115)  mas / a
Physical Properties
Dimensions 1.2 ± 0.2 / 0.29 ± 0.04  M ☉
Rotation time 3.316825 h
Other names
and catalog entries
2MASS catalog 2MASS J18485464 + 0035030 [1]
Other names Nova Aql. 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, EM * RJHA 116, HBHA 202-05, PLX 4341, AAVSO 1843 + 00.

Template: Infobox star / maintenance / magGTemplate: Infobox star / maintenance / magJ

Nova Aquilae 1918 or V603 Aquilae was a very bright nova with a maximum brightness of −0.5 m , which lit up in 1918 in the constellation Eagle .

After the maximum, the star system showed a decrease in brightness of three magnitudes within 12 days and is therefore assigned to the very fast novae of the NA type. It had faded again by about 1/100 of an order of magnitude to an average apparent magnitude of 11.43 m every decade since the 1940s .

The Nova was discovered on June 7, 1918 by the Polish amateur astronomer , doctor and professor of anatomy at the University of Geneva Zygmunt Laskowski , and confirmed on the following nights by George Noel Bower, Alice Grace Cook and many others. With a magnitude of −0.5 m , it was the brightest nova that had been discovered since the telescope was first discovered in 1608, and therefore - except for Sirius and Canopus - brighter than all other stars in the night sky.

Johann Georg Hagen Director of the Vatican Observatory near Castel Gandolfo reported on August 15, 1918 that the light fluctuations of the Nova Aquilae from 1918, as reported in the previous issues of Astronomical News, partly when it was lit between June 5 and 15, but specifically in the earlier years, when in 1888 the size 11.0 m , then in 1895 the size 9.3 m and between 1906 and 1917 the sizes 10.2 m to 10.5 m were assigned, the older reports about a "New Star" in the constellation Adler, which is said to have appeared before 1592, given increased importance.

In 1964, Robert Paul Kraft established that Nova Aquilae 1918, as well as the Novae GK Persei , T Aurigae , T Coronae Borealis , DQ Herculis , and WZ Sagittae are binary systems.

A published in 1999 by J. Arenas et al. Spectroscopic analysis carried out at Keele University showed that Nova Aquilae 1918 is a cataclysmically variable binary star system consisting of a white dwarf with an accretion disk of about 1.2 ± 0.2 M ☉ and a hot subdwarf with about 0.29 ± 0 , 04 M ☉ is that a surface temperature of about 10,000 K has. Both orbit each other in close orbit with a period of 3 hours and 19.5 minutes.

Individual evidence

  1. ↑ a b c d e f g V * V603 Aql. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed April 10, 2019 .
  2. ↑ a b c d V0603 Aql. In: VSX. AAVSO , accessed April 10, 2019 .
  3. ↑ HIP 92316. In: Gaia DR1. VizieR , accessed April 10, 2019 .
  4. ↑ Hubble space telescope fine guidance sensor parallaxes for four classical novae. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed April 11, 2019 .
  5. ↑ a b Johnson, Christopher B .; Schaefer, Bradley E .; Kroll, Peter; Henden, Arne A .: Nova Aquilae 1918 (V603 Aql) Faded by 0.44 mag / century from 1938-2013 . In: The Astrophysical Journal . 780, No. 2, 2013, p. L25. arxiv : 1310.6802 . bibcode : 2014ApJ ... 780L..25J . doi : 10.1088 / 2041-8205 / 780/2 / L25 .
  6. ^ HW Duerbeck: The final decline of novae and the hibernation hypothesis . In: Monthly Notices of the Royal Astronomical Society, Volume 258, Issue 3, 1 October 1992, Pages 629-638, . April 11, 2019.
  7. ↑ Biographical Notes on George Noel Bower (1885-1951). In: Bill Barton, FRAS. Orwell Astronomical Society Ipswich, accessed April 10, 2019 .
  8. ↑ Patrick Moore: The Amateur Astronomer . Springer, 2006, ISBN 978-1846282867 , p. 145.
  9. ↑ The older literature on a "New Star" in Aquila and the name of the Novae. In: Hagen, JG Astronomische Nachrichten, volume 208, Issue 5, p.67, accessed on April 10, 2019 .
  10. ^ A b Robert P. Kraft: Binary stars among cataclysmic variables. III. Ten old novae . In: Astrophysical Journal . 139, 1964, pp. 457-75. bibcode : 1964ApJ ... 139..457K . doi : 10.1086 / 147776 .
  11. ↑ Arenas, J .; Catalan, MS; Augusteijn, T .; Retter, A .: A spectroscopic study of V603 Aquilae: stellar parameters and continuum-line variations . In: Monthly Notices of the Royal Astronomical Society . 311, No. 1, 2000, pp. 135-48. bibcode : 2000MNRAS.311..135A . doi : 10.1046 / j.1365-8711.2000.03061.x .