T Pyxidis

T Pyxidis

T Pyx surrounded by the nova remnants of a previous outburst. Hubble Space Telescope composite
Observation data
Epoch J2000      Equinox J2000
Constellation Pyxis
Right ascension 09h 04m 41.5062s[1]
Declination −32° 22′ 47.5033″[1]
Apparent magnitude (V) 6.4 Max.
18.5 Min.[2]
Characteristics
Spectral type White Dwarf
Variable type Recurrent nova[2]
Astrometry
Proper motion (μ) RA: −2.531±0.052[1] mas/yr
Dec.: 0.177±0.062[1] mas/yr
Parallax (π)0.3051 ± 0.0419 mas[1]
Distance3185+607
−283[2] pc
Details
White dwarf
Mass0.7±0.2 M☉
Second component
Mass0.14±0.03 M☉
Orbit
Period (P)1.8295 hours
Inclination (i)10±2°
Other designations
Nova Pyx 1890, AAVSO 0900-31, Gaia DR2 5628258258606112768, 2MASS J09044150-3222474[3]
Database references
SIMBADdata
The location of T Pyxidis (circled in red).

T Pyxidis (T Pyx)[4] is a recurrent nova[5] and nova remnant in the constellation Pyxis. It is a binary star system and its distance is estimated at 4,783 parsecs (15,600 light-years) from Earth. It contains a Sun-like star and a white dwarf. Because of their close proximity and the larger mass of the white dwarf, the latter draws matter from the larger, less massive star. The influx of matter on the white dwarf's surface causes periodic thermonuclear explosions to occur.

The usual apparent magnitude of this star system is 15.5, but there have been observed eruptions with maximal apparent magnitude of about 7.0 in the years 1890, 1902, 1920, 1944, 1966 and 2011.[6] Evidence seems to indicate that T Pyxidis may have increased in mass despite the nova eruptions, and is now close to the Chandrasekhar limit when it might explode as a supernova.[7] When a white dwarf reaches this limit it will collapse under its own weight and cause a type Ia supernova.

  1. ^ a b c d e Cite error: The named reference Gaia DR2 was invoked but never defined (see the help page).
  2. ^ a b c Cite error: The named reference Schaefer2018 was invoked but never defined (see the help page).
  3. ^ Cite error: The named reference Simbad was invoked but never defined (see the help page).
  4. ^ According to the Argelander system of nomenclature for variable stars, the initial letter is an R, and the counter progresses alphabetically. Thus, T Pyx is the third variable star in the constellation Pyx.
  5. ^ Shara, Michael M.; Zurek, David R.; Williams, Robert E.; Prialnik, Dina; et al. (June 1997). "HST Imagery of the Non-Expanding, Clumped "Shell" of the Recurrent Nova T Pyxidis". Astronomical Journal. 114 (1): 258. Bibcode:1997AJ....114..258S. doi:10.1086/118470.
  6. ^ "Outburst of the recurrent nova T Pyx". AAVSO. 2011.
  7. ^ "T Pyxidis Soon To Be A Type Ia Supernova". Space Daily. 2010-01-05. Retrieved 2010-01-05.