Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Leo |
Right ascension | 11h 17m 15.92381s [2] |
Declination | +17° 57′ 41.6804″ [2] |
Apparent magnitude (V) | 17.5-19 [3] |
Characteristics | |
Variable type | AM Her [3] |
Astrometry | |
Radial velocity (Rv) | 0.0 [4] km/s |
Proper motion (μ) |
RA: −28.700
mas/
yr
[2] Dec.: −1.444 mas/ yr [2] |
Parallax (π) | 3.2781 ± 0.3110 mas [2] |
Distance | 990 ± 90
ly (310 ± 30 pc) |
Orbit | |
Period (P) | 0.0623628426 [5] yr |
Eccentricity (e) | 0.0 (fixed) |
Inclination (i) | 79.5 [6]° |
Details | |
White dwarf | |
Mass | 0.6 [6] M☉ |
Temperature | 13,500 [5] K |
Donor star | |
Mass | 0.09 [6] M☉ |
Other designations | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
DP Leonis (abbreviated DP Leo) is a binary star system in the equatorial constellation of Leo. It is a variable star that ranges in apparent visual magnitude from 17.5 down to 19. [3] The system is located at a distance of approximately 990 light-years from the Sun based on parallax. [2] It is a cataclysmic variable star of the AM Herculis-type also known as polars. The system comprises an eclipsing white dwarf and red dwarf in tight orbit (nearly 1.5 hours) and an extrasolar planet. [8] This eclipsing variable was discovered by P. Biermann and associates in 1982 as the optical counterpart to the EINSTEIN X-ray source E1114+182. [9]
In 2010, Qian et al. announced the detection of a third body of planetary mass around the eclipsing binary system. The presence of a third body had already been suspected in 2002. [6] The object is roughly 6 times more massive than Jupiter and is located 8.6 AU from the binary.
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( years) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | ≥6.1 ± 0.5 MJ | 8.2 ± 0.4 | 28.0 ± 2.0 | 0.39 ± 0.13 | — | — |