PDS 110

PDS 110 is a young 11th magnitude star located approximately 1,090 light-years (335 pc)[2] away in the constellation Orion. In 2017, it was discovered that the star is orbited by an exoplanet or brown dwarf with a disk of dust around it.

PDS 110

PDS 110
Credit: Two Micron All Sky Survey (2MASS)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Orion
Right ascension 05h 23m 31.008s
Declination –01° 04′ 23.68″
Apparent magnitude (V) 10.4
Characteristics
Spectral type keF6IVeb[1][2]
Astrometry
Proper motion (μ) RA: 1.146 ± 1.067[2] mas/yr
Dec.: −0.338 ± 1.076[2] mas/yr
Parallax (π)2.91 ± 0.34[2] mas
Distance1035[2] ly
(335[2] pc)
Absolute magnitude (MV)+2.54[2]
Details
Mass3.0[3] M☉
Radius2.23[2] R☉
Luminosity (bolometric)7.76[2] L☉
Surface gravity (log g)3.8[2] cgs
Temperature6,653[3] K
Metallicity [Fe/H]+0.06[2] dex
Age10[3] Myr
Other designations
HD 290380, IRAS 05209-0107, GLMP 91, 2MASS J05233100-0104237, TYC 4753-1534-1
Database references
SIMBADdata

Description

PDS 110 is a young star still approaching the main sequence. It has been classified as a T Tauri star,[4] or as a pre-main sequence star.[3] 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.[3]

Dust disk around secondary object
The PDS 110 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 1.8-70 MJ 2 808 ± 2 — — —

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. Another transit was predicted for September 2017,[2] but nothing similar to the previous events was seen, ruling out a periodic event.[5]


See also

References
  1. Miroshnichenko, A. S.; Gray, R. O.; Vieira, S. L. A.; Kuratov, K. S.; Bergner, Yu. K. (1999). "Observations of recently recognized candidate Herbig Ae/Be stars". Astronomy and Astrophysics. 347: 137. Bibcode:1999A&A...347..137M.
  2. Osborn, H. P.; et al. (2017). "Periodic Eclipses of the Young Star PDS 110 Discovered with WASP and KELT Photometry". Monthly Notices of the Royal Astronomical Society. 471 (1): 740–749. arXiv:1705.10346. Bibcode:2017MNRAS.471..740O. doi:10.1093/mnras/stx1249. S2CID 119450480.
  3. Rojas, G.; Gregorio-Hetem, J.; Hetem, A. (2008). "Towards the main sequence: Detailed analysis of weak line and post-T Tauri stars". Monthly Notices of the Royal Astronomical Society. 387 (3): 1335. Bibcode:2008MNRAS.387.1335R. doi:10.1111/j.1365-2966.2008.13355.x.
  4. Gregorio-Hetem, J.; Hetem, A. (2002). "Classification of a selected sample of weak T Tauri stars". Monthly Notices of the Royal Astronomical Society. 336 (1): 197–206. Bibcode:2002MNRAS.336..197G. doi:10.1046/j.1365-8711.2002.05716.x.
  5. PDS 110 Observing Campaign - Monitoring the potential September 2017 eclipse of young star PDS 110.
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