X Persei ( X Persei ) is a massive X-ray binary star in the constellation Perseus , located at a distance of about 950 pc from the Sun.
| X Perseus | |||
|---|---|---|---|
| Star | |||
 | |||
| Observational data ( Epoch J2000.0 ) | |||
| Right ascension | |||
| Declination | |||
| Distance | 950 pc [2] | ||
| Visible magnitude ( V ) | 6,778 [3] (6.03 - 7.00 [4] ) | ||
| Constellation | Perseus | ||
| Astrometry | |||
| Radial velocity ( R v ) | −50.00 [5] km / s | ||
| Proper motion (μ) | RA: −1,330 [1] mas per year Dec: −1.743 [1] mas per year | ||
| Parallax (π) | 1.38 [1] ± 0.48 mas | ||
| Absolute magnitude (V) | −3.47 [3] | ||
| Specifications | |||
| Spectral class | O9.5IIIe-B0Ve [6] | ||
| Color Indicator ( B - V ) | +0.137 [3] | ||
| Color Index ( U - B ) | −0.790 [3] | ||
| Variability | γ Cas + X-ray pulsar [4] | ||
| physical characteristics | |||
| Weight | 15.5 [7] M ☉ | ||
| Radius | 6.5 [7] R ☉ | ||
| Age | 5 million [3] years | ||
| Temperature | 29500 [7] K | ||
| Luminosity | 29000 [3] L ☉ | ||
| Rotation | 215 km / s [3] | ||
| |||
| Information in databases | |||
| SIMBAD | data | ||
The optical component X of Perseus belongs to the class of giants of the spectral class O or to the stars of the main sequence of the spectral class B. The object is a rapidly rotating Be-star , probably surrounded by a disk of ejected material. According to such features, a star can be attributed to variables of the Gamma type of Cassiopeia ; The apparent magnitude varies from 6 to 7. In 1989 and 1990, the spectrum of the star changed from the spectrum of a Be-star to the spectrum of an ordinary star of spectral class B, while the star weakened its brightness. This phenomenon was probably due to the disappearance of the accretion disk. Since that time, the disk has been formed again and shows powerful emission lines. [eight]
Perseus's X is drawn next to a neutron star , noted in the Uhuru X-ray Object Catalog as 4U 0352 + 309. The neutron star is a pulsar with an unusually large period of 837 seconds. [9] The pulsar exhibits a change in the pulsation period associated with the transfer of matter from a more massive star. Between 1973 and 1979, an increase in rotational speed was observed, associated with a powerful X-ray flash and likely mass transfer. Since then, the overall rotational speed has decreased, despite a series of small x-ray flashes. [eight]
Since the binary system consists of a neutron star and an OB star with emission lines, it is classified as Be / X-ray binary stars. [eight]
The binary system has an optical companion divided by a distance of 22.5 "and called Perthus B. in the Component Catalog of Binary and Multiple Stars X. [10]
Notes
- ↑ 1 2 3 4 5 Gaia Collaboration; Brown, AG A; Vallenari, A; Prusti, T; De Bruijne, JH J; Mignard, F; Drimmel, R; Babusiaux, C; Bailer-Jones, CA L; Bastian, U; Biermann, M; Evans, D. W; Eyer, L; Jansen, F; Jordi, C; Katz, D; Klioner, S. A; Lammers, U; Lindegren, L; Luri, X; O'Mullane, W; Panem, C; Pourbaix, D; Randich, S; Sartoretti, P; Siddiqui, H. I; Soubiran, C; Valette, V; Van Leeuwen, F; Walton, NA Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties (English) // Astronomy & Astrophysics. - 2016. - Vol. 595 . - P. A2 . - DOI : 10.1051 / 0004-6361 / 201629512 . - . - arXiv : 1609.04172 .
- ↑ Walter, Roland; Lutovinov, Alexander A .; Bozzo, Enrico; Tsygankov, Sergey S. High-mass X-ray binaries in the Milky Way. A closer look with INTEGRAL (Eng.) // The Astronomy and Astrophysics Review. - 2015. - Vol. 23 . - P. 2 . - DOI : 10.1007 / s00159-015-0082-6 . - . - arXiv : 1505.03651 .
- ↑ 1 2 3 4 5 6 7 Lyubimkov, LS; Rostopchin, SI; Roche, P .; Tarasov, AE Fundamental parameters, helium abundance and distance of X Persei (English) // Monthly Notices of the Royal Astronomical Society. - 1997. - Vol. 286 , no. 3 - P. 549 . - DOI : 10.1093 / mnras / 286.3.549 . - .
- ↑ 1 2 Samus, NN; Durlevich, OV VizieR Online Data Catalog: General Catalog of Variable Stars (Samus + 2007-2013) (English) // VizieR On-line Data Catalog: B / gcvs. Originally published in: 2009yCat .... 102025S. - 2009. - Vol. 1 . - .
- ↑ Kharchenko, NV; Scholz, R.-D .; Piskunov, AE; Röser, S .; Schilbach, E. Astrophysical supplements to the ASCC-2.5: Ia. Galactic open clusters and associations (English) // Radial velocities of ˜55000 stars and mean radial velocities of 516 // Astronomische Nachrichten. - 2007. - Vol. 328 , no. 9 - P. 889 . - DOI : 10.1002 / asna.2007 .10776 . - . - arXiv : 0705.0878 .
- ↑ Valencic, Lynne A .; Smith, Randall K. Interstellar Abundances towards X Per, Revisited (Eng.) // The Astrophysical Journal. - 2013. - Vol. 770 . - P. 22 . - DOI : 10.1088 / 0004-637X / 770/1/22 . - .
- ↑ 1 2 3 Grundstrom, ED; Boyajian, TS; Finch, C .; Gies, DR; Huang, W .; McSwain, MV; O'Brien, DP; Riddle, rl; Trippe, ML; Williams, SJ; Wingert, DW; Zaballa, RA Joint Hα and X-Ray Observations of Massive X-Ray Binaries. Iii. The Be X-Ray Binaries HDE 245770 = A0535 + 26 and X Persei (Eng.) // The Astrophysical Journal. - 2007. - Vol. 660 , no. 2 - P. 1398 . - DOI : 10.1086 / 514325 . - . - arXiv : astro-ph / 0702283 .
- ↑ 1 2 3 Li, Hui; Yan, Jingzhi; Zhou, Jianeng; Liu, Qingzhong. Binary X Per (English) // The Astronomical Journal. - 2014. - Vol. 148 , no. 6 - P. 113 . - DOI : 10.1088 / 0004-6256 / 148/6/113 . - . - arXiv : 1408.3542 .
- ↑ Delgado-Marti, H .; Levine, AM; Pfahl, E .; Rappaport, SA The Orbit of X Persei and Its Neutron Star Companion (eng.) // The Astrophysical Journal. - 2001. - Vol. 546 . - P. 455 . - DOI : 10.1086 / 318236 . - . - arXiv : astro-ph / 0004258 .
- ↑ Dommanget, J .; Nys, O. Catalog des composantes d'étoiles doubles (CCDM) first edition ( CCDM) first edition (Eng.) // Com. de l'Observ. Royal de Belgique. - 1994. - Vol. 115 - P. 1 . - .