Pshibylsky Star ( HD 101065 ) is a peculiar star that is located about 410 light-years from the Sun in the constellation Centaurus .
| Pshibylsky Star | |||
|---|---|---|---|
| Star | |||
| Observational data ( Age J2000.0 ) | |||
| Type of | Peculiar star | ||
| Right ascension | |||
| Declination | |||
| Distance | 410.08 ± 48.64 St. years (125.79 ± 14.92 pc ) [one] | ||
| Visible magnitude ( V ) | V max = +8.02 m , V min = +7.99 m , P = 0.0084306 d [2] | ||
| Constellation | Centaurus | ||
| Astrometry | |||
| Radial velocity ( R v ) | 10.2 [3] km / s | ||
| Own movement (μ) | RA: -47.30 [3] Dec: 33.93 [3] | ||
| Parallax (π) | 7.9 ± 51.07 [3] mas | ||
| Absolute magnitude (V) | V max = 2.52 m , V min = 2.49 m , P = 0.0084306 d [4] | ||
| Specifications | |||
| Spectral class | B5p [3] | ||
| Color Index ( B - V ) | 0.762 [1] | ||
| Color Index ( U - B ) | 0.20 [3] | ||
| physical characteristics | |||
| Weight | 0.87 [1] M ☉ | ||
| Radius | 3.46 ± 0.64 [1] R ☉ | ||
| Temperature | 5 380.00 ± 100 [1] K | ||
| Luminosity | 8.985 ± 2.699 [1] L ☉ | ||
| Metallicity | 630% [3] | ||
| The properties | roap star | ||
| |||
| Database Information | |||
| SIMBAD | data | ||
In 1961, the Polish-Australian astronomer Antonin Pshibylsky discovered that this star has a peculiar spectrum that does not fit into the standard framework of stellar classification . Pshibylsky's observations showed an unusually low amount of iron and nickel in the spectrum of the star and a large number of rare elements such as strontium , niobium , scandium , yttrium , cesium , neodymium , praseodymium , thorium , ytterbium, and uranium . At first, Pshibylsky doubted that iron was generally present in the spectrum. Modern work shows that the elements of the iron group are still present in amounts slightly below normal, but it is also clear that the amount of lanthanides and other exotic elements is extremely excessive. As a result, these peculiar stars are distinguished into a separate class of Ap stars [5] .
The following radioactive elements were also found in the Pshibylsky star: technetium , promethium , sea anemone , protactinium , neptunium , plutonium , americium , curium , berkeley , California , einstein [6] .
The Pshibylsky star is apparently a main sequence star or subgiant . In addition to the usual lines of singly ionized calcium (Ca II) H and K, the spectrum of HD 101065 contains strong lines of singly ionized lanthanides , and in this way it resembles S stars whose atmospheres are enriched with recently synthesized matter that has risen from their bowels [7] .
Several hypotheses have been proposed to explain the unusual properties of the Pshibylsky star. The first is that it is a cold extreme star of the Ap class. This theory is confirmed by the discovery in HD 101065 of a magnetic field with a strength of several kilogauss , which makes it similar to many other Ap stars. However, one of the unresolved difficulties in interpreting HD 101065 as an Ap class star is that its spectrum is not similar to the spectrum of other Ap stars. The lines of neutral and ionized iron in the spectra of Ap stars are strong, and in some cases there is a clear excess of iron, which is not the case with the Pshibylsky star [8] . In 2008, Ukrainian scientists proposed another hypothesis to explain the properties of the Pshibylsky star. Its authors claim that the star has a satellite - a pulsar . Under the influence of its x-ray and electron-positron radiation, thermonuclear reactions occur in the atmosphere of the Pshibylsky star. As a result of this, heavy elements, which are usually formed only during supernova explosions , are synthesized in this star in the upper atmosphere [9] . However, the presence of a nearby massive pulsar satellite is not confirmed by modern radial velocity data of the star.
Quick Oscillations
HD 101065 is a prototype of roAp class stars . In 1978, according to photometric observations, it was found that the star pulsates with a period of 12.15 minutes [2] . Based on precision measurements of the radial velocities of the stars obtained with the HARPS spectrometer at the 3.6-meter telescope of the South European Observatory, a multi-periodic pulsation spectrum was discovered, showing the distance between the pulsation frequencies characteristic of high-overtone acoustic vibrations [10] . Modeling the frequency splitting made it possible to determine the exact parameters and age of the star and the magnitude of its magnetic field.
Notes
- ↑ 1 2 3 4 5 6 Object and Aliases (inaccessible link) . NASA / IPAC / NExSci Star & Exo Planet Observations . Archived on May 5, 2012.
- ↑ 1 2 Kurtz, DW Information Bulletin on Variable Stars, vol 1436, 1978 (inaccessible link) . Date accessed August 4, 2010. Archived October 3, 2018.
- ↑ 1 2 3 4 5 6 7 V * V816 Cen - Variable Star . SIMBAD Center de Données astronomiques de Strasbourg. Archived on May 5, 2012.
- ↑ From apparent magnitude and parallax
- ↑ Przybylski, A .; Kennedy, PM The Spectrum of HD 101065 (Eng.) // Publications of the Astronomical Society of the Pacific . - 1963. - Vol. 74 , no. 445 . - P. 349-353 . - DOI : 10.1086 / 127965 . (eng.)
- ↑ Gopka, VF; Yushchenko, AV; Yushchenko, VA; Panov, IV; Kim, Ch. Identification of absorption lines of short half-life actinides in the spectrum of Przybylski's star (HD 101065) (Russian) // Kinematics and Physics of Celestial Bodies: journal. - 2008 .-- 15 May ( vol. 24 , no. 2 ). - P. 89-98 . - DOI : 10.3103 / S0884591308020049 . - .
- ↑ Przybylski's Most Unusual Star (inaccessible link) . C. Cowley . Archived on May 5, 2012.
- ↑ Przybylski's Star (HD 101065 ) . Encyclopedia of Astrobiology, Astronomy, and Spaceflight . Archived on May 5, 2012.
- ↑ A hypothesis for explaining the origin of Przybylski's star (HD 101065 ) . VF Gopka, OM Ul'yanov and SM Andrievskii .
- ↑ DE Mkrtichian, AP Hatzes, H. Saio, RR Shobbrook. [ http://adsabs.harvard.edu/abs/2008A&A...490.1109M The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star] (Eng.) // Astronomy and Astrophysics . - EDP Sciences 2008-09-17. - Vol. 490 , iss. 3 . - P. 1109-1120 . - ISSN 1432-0746 0004-6361, 1432-0746 . - DOI : 10.1051 / 0004-6361: 200809890 .