Langbahn Team – Weltmeisterschaft

PDS 110

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 31.01018s[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]
Distance1,130 ± 8 ly
(347 ± 3 pc)
Absolute magnitude (MV)+2.54[3]
Details
Mass3.0[5] M☉
Radius2.23[3] R☉
Luminosity (bolometric)7.76[3] L☉
Surface gravity (log g)3.8[3] cgs
Temperature6,653[5] K
Metallicity [Fe/H]+0.06[3] dex
Age10[5] Myr
Other designations
HD 290380, IRAS 05209-0107, GLMP 91, 2MASS J05233100-0104237, TYC 4753-1534-1
Database references
SIMBADdata

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]

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

light curves for PDS 110 showing the 2008 and 2011 eclipses, adapted from Osborn et al. (2017)[3]

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]

See also

References

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ 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.
  3. ^ a b c d e f g h i 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.
  4. ^ a b c d Osborn, H. P.; Kenworthy, M.; et al. (May 2019). "The PDS 110 observing campaign - photometric and spectroscopic observations reveal eclipses are aperiodic". Monthly Notices of the Royal Astronomical Society. 485 (2): 1614–1625. arXiv:1901.07981. Bibcode:2019MNRAS.485.1614O. doi:10.1093/mnras/stz283.
  5. ^ a b c d e 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.
  6. ^ 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.
  7. ^ PDS 110 Observing Campaign - Monitoring the potential September 2017 eclipse of young star PDS 110.
  8. ^ Pinheiro, Tiago F. L. L.; Sfair, Rafael (August 2021). "Constraining the nature of the possible extrasolar PDS110b ring system". Astronomy & Astrophysics. 652: A149. arXiv:2107.05179. Bibcode:2021A&A...652A.149P. doi:10.1051/0004-6361/202039556.
Quelle: http://en.wikipedia.org/wiki/PDS_110