GK Persei (also Nova Persei 1901) was a bright nova first observed on Earth in 1901. It was discovered by Thomas David Anderson, an Edinburgh clergyman, at 02:40 UT on 22 February 1901 when it was at magnitude 2.7.[9][10] It reached a maximum magnitude of 0.2, the brightest nova of modern times until Nova Aquilae 1918. After fading into obscurity at about magnitude 12 to 13 during the early 20th century, GK Persei began displaying infrequent outbursts of 2 to 3 magnitudes (about 7 to 15 times quiescent brightness). Since about 1980, these outbursts have become quite regular, typically lasting about two months and occurring about every three years. Thus, GK Persei seems to have changed from a classical nova like Nova Aquilae 1918 to something resembling a typical dwarf nova-type cataclysmic variable star.
 GK Persei and the surrounding Firework Nebula. | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 03h 31m 11.82s[1] |
| Declination | +43° 54′ 16.8″[1] |
| Apparent magnitude (V) | 0.02[2] - 14.0[3] |
| Characteristics | |
| Spectral type | K1IV[4] |
| Astrometry | |
| Radial velocity (Rv) | 5.5[5] km/s |
| Proper motion (μ) | RA: −6.878[6] mas/yr Dec.: −17.348[6] mas/yr |
| Parallax (π) | 2.3063 ± 0.0415 mas[6] |
| Distance | 1,440+29 −26 ly (442+9 −8[2] pc) |
| Absolute magnitude (MV) | −9.1 - +3.7[2] |
| Orbit[7] | |
| Period (P) | 1.996872 ± 0.000009 d |
| Inclination (i) | 67 ± 5° |
| Semi-amplitude (K2) (secondary) | 126.4 ± 0.9 km/s |
| Details[7] | |
| White dwarf | |
| Mass | 1.03+0.16 −0.11 M☉ |
| Subgiant | |
| Mass | 0.39+0.07 −0.06 M☉ |
| Radius | 2.26 ± 0.11 R☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
Surrounding GK Persei is the Firework Nebula, a nova remnant first detected in 1902 consisting of an expanding cloud of gas and dust bubbles moving up to 1200 km/s.[11]
GK Persei has precise parallaxes reported from Gaia DR2 and Gaia EDR3,[12][6] but these are thought to be badly affected by the binary nature of the system. The Hubble Space Telescope has used a different method to derive the distance to GK Persei using nebular expansion velocity and compares that with its own astrometric parallax calculation. This gave a somewhat smaller parallax (larger distance) than the Gaia measurements.[13]
Properties
editNovae consist of a main-sequence to giant star that accretes mass onto a white dwarf. The two stars of GK Persei orbit each other with a period of nearly 2 days. The white dwarf, with a mass of 1.03 M☉, has one of the highest masses measured in a cataclysmic variable. The donor star, having donated much of its mass to the white dwarf, is only 0.39 M☉ despite being a subgiant star.[7]
Gallery
edit-
The location of GK Persei (circled in red) -
GK Persei by the 32-inch Schulman Telescope at the Mt. Lemmon Observatory. -
Expanding Nebula around GK Persei. Images range from 1953 to 2012. -
Changing light-echo observed at the time of the 1901 Nova, hand-drawn by G.W. Ritchey at the Yerkes Observatory.
References
edit- ^ a b Downes, Ronald; Webbink, Ronald F.; Shara, Michael M. (April 1997), "A Catalog and Atlas of Cataclysmic Variables-Second Edition", Publications of the Astronomical Society of the Pacific, 109: 345–440, Bibcode:1997PASP..109..345D, doi:10.1086/133900, S2CID 120396435
- ^ a b c Schaefer, Bradley E. (December 2018). "The distances to Novae as seen by Gaia". Monthly Notices of the Royal Astronomical Society. 481 (3): 3033–3051. arXiv:1809.00180. Bibcode:2018MNRAS.481.3033S. doi:10.1093/mnras/sty2388. S2CID 118925493.
- ^ van Altena, William F.; Lee, J.T.; et al. (1995). The general catalogue of trigonometric [stellar] parallaxes. Bibcode:1995gcts.book.....V.
- ^ Morales-Rueda, L.; Still, M.D.; Roche, P.; Wood, J.H.; Lockley, J.J. (January 2002). "The stellar mass ratio of GK Persei". Monthly Notices of the Royal Astronomical Society. 329 (3): 597–604. arXiv:astro-ph/0110332. Bibcode:2002MNRAS.329..597M. doi:10.1046/j.1365-8711.2002.05013.x.
- ^ Wilson, Ralph Elmer (January 1953). "General catalogue of stellar radial velocities". Carnegie Institute Washington D.C. Publication. Bibcode:1953GCRV..C......0W. Retrieved 25 January 2021.
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c Álvarez-Hernández, A.; Torres, M A P.; Rodríguez-Gil, P.; Shahbaz, T.; Anupama, G. C.; Gazeas, K. D.; Pavana, M.; Raj, A.; Hakala, P.; Stone, G.; Gomez, S.; Jonker, P. G.; Ren, J-J; Cannizzaro, G.; Pastor-Marazuela, I.; Goff, W.; Corral-Santana, J. M.; Sabo, R. (2021). "The intermediate polar cataclysmic variable GK Persei 120 years after the nova explosion: A first dynamical mass study". Monthly Notices of the Royal Astronomical Society. 507 (4): 5805–5819. arXiv:2107.06932. doi:10.1093/mnras/stab2547.
- ^ "V* GK Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 28 December 2016.
- ^ Shears, Jeremy (2012). "The astronomizings of Dr. Anderson and the curious case of his disappearing nova". The Journal of the British Astronomical Association. 123 (5): 270–279. arXiv:1209.4057. Bibcode:2013JBAA..123..270S.
- ^ Warner, B. (February 2006). "Where have all the novae gone?". Astronomy & Geophysics. 47 (1): 29–32. Bibcode:2006A&G....47a..29W. doi:10.1111/j.1468-4004.2006.47129.x.
- ^ "NOAO". Archived from the original on 28 May 2010. Retrieved 22 June 2008.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ 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. S2CID 118376206.