PDS 110

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PDS 110
2MASS J05233100-0104237.png
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

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]

Contents

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) PDS110LightCurve.png
light curves for PDS 110 showing the 2008 and 2011 eclipses, adapted from Osborn et al. (2017)

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. 1 2 3 4 5 6 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. 1 2 3 4 5 6 7 8 9 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. 1 2 3 4 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. 1 2 3 4 5 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.
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