GK Persei

from Wikipedia, the free encyclopedia
Double star
GK Persei
Overlay of images of the Nova GK Persei in the X-ray range, blue, in the optical range, yellow and in the radio wave range, pink; created from images from the Chandra Space Telescope, the Hubble Space Telescope and the Very Large Array
Overlay of images of the Nova GK Persei in the X-ray range, blue, in the optical range, yellow and in the radio wave range, pink; created from images from the Chandra Space Telescope , the Hubble Space Telescope and the Very Large Array
AladinLite
Observation
dates equinox :  J2000.0 , epoch : J2000.0
Constellation Perseus
Right ascension 03 h 31 m 12.01 s
declination + 43 ° 54 ′ 15.5 ″
Apparent brightness 14.0 mag
Typing
Spectral class WD + K2 IVe
Variable star type NA / DQ + UG 
Astrometry
Radial velocity (5.7 ± 2) km / s
parallax (2.26 ± 0.04)  mas
distance (1,450)  ly
(440)  pc
Proper movement 
Rec. Share: (−6.71 ± 0.08)  mas / a
Dec. portion: (−17.19 ± 0.07)  mas / a
Physical Properties
Dimensions (0.87 ± 0.08 /?)  M ☉
Effective temperature (5100)  K
Metallicity [Fe / H] (−0.125)
Other names
and catalog entries
Bonn survey BD + 43 ° 740a
Bright Star Catalog HR 1057 [1]
Henry Draper Catalog HD 21629 [2]
2MASS catalog 2MASS J03311201 + 4354154 [3]
Other names GK Persei, Nova Persei 1901

GK Persei (also Nova Persei 1901 ) was a nova that lit up in 1901 in the constellation Perseus and with a maximum brightness of 0.2  mag was one of the brightest novas observed in modern times. As a nova remnant, with a brightness of 13.5 mag, GK Persei is a cataclysmic variable (CV) that combines a number of properties that rarely occur in this combination: The orbital period of GK Persei is 1.99 days the longest observed in CVs, and the companion star is a subgiant and not, as is usually the case, a main sequence star . The accreting white dwarf is magnetic and rotates with a period of 351 seconds, which means that GK Persei can be assigned to the asynchronous, magnetic CVs of the DQ-Herculis type.

In addition, dwarf nova outbreaks are observed in GK Persei , during which the brightness of the system increases by 2 to 3 magnitudes. The outbreaks occur approximately 3 years apart and last approximately 2 months.

GK Persei is surrounded by an expanding shell that stems from the last nova eruption and is sometimes referred to as a fireworks nebula .

reception

In his short story Beyond the Wall of Sleep (German: Beyond the Wall of Sleep ), the American writer processed HP Lovecraft , the Nova Persei as a short story in which an alien being in the body of a man out for revenge on the star Algol muses.

Web links

Commons : GK Persei  - collection of pictures, videos and audio files

Individual evidence

  1. ↑ a b c d e f g GK Per. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed August 26, 2018 .
  2. ↑ a b GK Per. In: VSX. AAVSO, accessed December 10, 2018 .
  3. ↑ Wada, Y. et al .: An Estimation of the White Dwarf Mass in the Dwarf Nova GK Persei with NuSTAR Observations of Two States . In: MNRAS . 474, No. 2, pp. 1564-1571. arxiv : 1711.01727 . bibcode : 2018MNRAS.474.1564W . doi : 10.1093 / mnras / stx2880 .
  4. ^ Crampton D., Fisher WA, Cowley AP: The orbit of GK Persei . In: The Astrophysical Journal . 300, 1986, p. 788. bibcode : 1986ApJ ... 300..788C . doi : 10.1086 / 163856 .
  5. ↑ Mauche CW: The Spin-Up Rate of the White Dwarf in GK Per . In: ASP Conference Proceedings . 315, 2004, p. 120. bibcode : 2004ASPC..315..120M .
  6. ^ "Beyond the Wall of Sleep." In: ST Joshi , David E. Schultz : An HP Lovecraft Encyclopedia. Greenwood Publishing Group, 2001; P. 19.