| |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lupus |
| Right ascension | 15h56m 41.88986s[1] |
| Declination | −42° 19′ 23.2746″[1] |
| Apparent magnitude (V) | 8.34[2] |
| Characteristics | |
| Spectral type | F6 III[2] |
| Astrometry | |
| Radial velocity (Rv) | -3.10[2] km/s |
| Proper motion (μ) | RA: -11.19[1] mas/yr Dec.: -24.46[1] mas/yr |
| Parallax (π) | 6.2791 ± 0.0284 mas[3] |
| Distance | 519 ± 2 ly (159.3 ± 0.7 pc) |
| Details | |
| Mass | 2.5 M☉ |
| Surface gravity (log g) | 3.15[4] cgs |
| Temperature | 6632[4] K |
| Metallicity [Fe/H] | 0.33[4] dex |
| Age | 1 Myr |
| Orbit[5] | |
| Primary | HD 142527 A |
| Companion | HD 142527 B |
| Semi-major axis (a) | 14.71+8.18 −2.33 AU |
| Eccentricity (e) | 0.28+0.22 −0.10 |
| Inclination (i) | 126.27+2.13 −2.28° |
| Longitude of the node (Ω) | 142.38+5.51 −6.12° |
| Periastron epoch (T) | 2021.07+0.82 −0.72 |
| Argument of periastron (ω) (secondary) | 86.02+52.31 −42.59° |
| Other designations | |
CD-41° 10447, HD 142527, HIP 78092, SAO 226389, WDS J15567-4219AB, 2MASS J15564188-4219232, TYC 846-688-1, Gaia DR2 5994826707951507200[2] | |
| Database references | |
| SIMBAD | data |
HD 142527 is a binary star system in the constellation of Lupus.[7][8] The primary star belongs to the Herbig Ae/Be star class, while the companion, discovered in 2012, is a red dwarf star or accreting protoplanet[5] with a projected separation of less than 0.1″.[9] The system is notable for its circumbinary protoplanetary disk and its discovery has helped refine models of planet formation. The orbit of companion is strongly inclined to the circumbinary protoplanetary disk.[5]
HD 142527 is listed in the International Variable star index as a UX Orionis variable, with a visible-light magnitude ranging from 8.27 to 8.60.[10]
HD 142527 is an extremely young star system, aged about 1 million years old[11] so it retains its protoplanetary disk, which has a mass of 15%ofthe Sun and a diameter of 980 AU.
Studies have shown eddies and vortex structures forming in the disk under the influence of two large planets.[12] The system is important as it allows astronomers to observe the accretion process in planetary formation.
In early 2013 an article was published by astronomers working with the ALMA telescope in Chile, which refers to the discovery of two massive flows of matter in the system.[13] Dust and gas is transferred from the periphery to the center through gravitational interaction with two giant planets that have a mass several times greater than the mass of Jupiter. Thus, the flows act as "pumps", pumping material from the edge of the center, "feeding" star. The planets themselves have not been detected so far, due to a dense shroud of gas. However, astronomers have proposed models that describe their existence.
Japanese astronomers have discovered particles of ice[14] in the disk.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| protoplanetary disk | 140–550 AU | 28° | — | |||
