PDS 110
Pre-main-sequence star
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PDS 110 is a young 11th magnitude star located approximately 1,130 light-years (350 parsecs) away in the constellation Orion. A series of eclipses was observed in 2008 and 2011, which may have been caused by dust from the star's circumstellar disk.[4]
PDS 110 Credit: Two Micron All Sky Survey (2MASS) | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Orion |
| Right ascension | 05h 23m 31.01018s[1] |
| Declination | −01° 04′ 23.7016″[1] |
| Apparent magnitude (V) | 10.4 |
| Characteristics | |
| Spectral type | keF6IVeb[2][3] |
| Variable type | UX Ori?[4] |
| Astrometry | |
| Radial velocity (Rv) | 27.97±2.55[1] km/s |
| Proper motion (μ) | RA: +1.503(19) mas/yr[1] Dec.: −0.388(12) mas/yr[1] |
| Parallax (π) | 2.8857±0.0212 mas[1] |
| Distance | 1,130 ± 8 ly (347 ± 3 pc) |
| Absolute magnitude (MV) | +2.54[3] |
| Details | |
| Mass | 3.0[5] M☉ |
| Radius | 2.23[3] R☉ |
| Luminosity (bolometric) | 7.76[3] L☉ |
| Surface gravity (log g) | 3.8[3] cgs |
| Temperature | 6,653[5] K |
| Metallicity [Fe/H] | +0.06[3] dex |
| Age | 10[5] Myr |
| Other designations | |
| HD 290380, IRAS 05209−0107, GLMP 91, 2MASS J05233100−0104237, TYC 4753-1534-1 | |
| Database references | |
| SIMBAD | data |
Description
PDS 110 is a young star still approaching the main sequence. It has been classified as a T Tauri star,[6] or as a pre-main sequence star.[5] The emission lines indicative of a T Tauri classification are somewhat weaker than a typical T Tauri star, interpreted as a post-T Tauri stage.[5]
PDS 110 hosts a circumstellar disk.[4]
2008-2011 eclipses
Brightness measurements from SuperWASP and KELT showed two similar reductions in brightness in November 2008 and January 2011, both with a maximal luminosity reduction of 30% and a duration of 25 days. These events were interpreted as transits of a structure with a period of 808 ± 2 days, corresponding to an orbital distance of about 2 AU. The large reduction in brightness could have happened due to a planet or brown dwarf with a circum-secondary disk of dust with a radius of 0.3 AU around a central object with a mass between 1.8 and 70 times the mass of Jupiter.[3]
Another transit was predicted for September 2017,[3] but nothing similar to the previous events was seen, ruling out a periodic event.[7] A search of 50 years of archival data also did not find any similar eclipses. The eclipses may have been caused by dust around PDS 110 itself. Larger-scale aperiodic dimmings have been observed as UX Orionis variables, and PDS 110 may be similar.[4]
An independent 2021 study, assuming that the eclipses were caused by a ringed object in orbit around the star, attempted to constrain the properties of such an object, with their preferred solution being a >35 MJ brown dwarf on a nearly circular orbit. However, this does not explain the fact that no eclipse was observed in 2017.[8]