HD 142527

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HD 142527
Artist’s impression of the disc and gas streams around HD 142527.jpg
Artist’s impression of the disc and gas streams around HD 142527
Observation data
Epoch J2000      Equinox J2000
Constellation Lupus
Right ascension 15h 56m 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[3] mas
Distance519 ± 2 ly
(159.3 ± 0.7 pc)
Details
Mass2.5 M☉
Surface gravity (log g)3.15[4] cgs
Temperature6632[4] K
Metallicity [Fe/H]0.33[4] dex
Age1 Myr
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
SIMBADdata

HD 142527 is a binary star system in the constellation of Lupus.[5][6] The primary star belongs to the Herbig Ae/Be star class, while the companion, discovered in 2012, is a red dwarf star with a projected separation of less than 0.1″.[7] The system is notable for its circumbinary protoplanetary disk and its discovery has helped refine models of planet formation.

Protoplanetary disk[]

HD 142527 is an extremely young star system, aged about 1 million years old[8] so it retains its protoplanetary disk, which has a mass of 15% of the of the 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.[9] 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.[10] 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[11] in the disk.

The planetary system[7]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
protoplanetary disk 140–550 AU 28° —

References[]

  1. ^ a b c d van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600. Vizier catalog entry
  2. ^ a b c d "HD 142527". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 5 January 2017.
  3. ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. Gaia EDR3 record for this source at VizieR.
  4. ^ a b c Luck, R. Earle (2015). "Abundances in the Local Region. I. G and K Giants". The Astronomical Journal. 150 (3): 88. arXiv:1507.01466. Bibcode:2015AJ....150...88L. doi:10.1088/0004-6256/150/3/88. S2CID 118505114.
  5. ^ "Hd 142527".
  6. ^ Simon Casassus, Gerrit van der Plas, Sebastian Perez M, William R. F. Dent, Ed Fomalont, Janis Hagelberg, Antonio Hales, Andrés Jordán, Dimitri Mawet, Francois Ménard, Al Wootten, David Wilner, A. Meredith Hughes, Matthias R. Schreiber, Julien H. Girard, Barbara Ercolano, Hector Canovas, Pablo E. Román & Vachail Salinas,Flows of gas through a protoplanetary gap, Nature 493, 191–194 (10 January 2013) .
  7. ^ a b Hunziker, S.; Schmid, H. M.; Ma, J.; Menard, F.; Avenhaus, H.; Boccaletti, A.; Beuzit, J. L.; Chauvin, G.; Dohlen, K.; Dominik, C.; Engler, N.; Ginski, C.; Gratton, R.; Henning, T.; Langlois, M.; Milli, J.; Mouillet, D.; Tschudi, C.; Van Holstein, R. G.; Vigan, A. (2021), "HD 142527: Quantitative disk polarimetry with SPHERE", Astronomy & Astrophysics, 648: A110, arXiv:2103.08462, Bibcode:2021A&A...648A.110H, doi:10.1051/0004-6361/202040166, S2CID 232233697
  8. ^ Hideaki Fujiwara, Mitsuhiko Honda, Hirokazu Kataza, Takuya Yamashita, Takashi Onaka, Misato Fukagawa, Yoshiko K. Okamoto, Takashi Miyata, Shigeyuki Sako, Takuya Fujiyoshi, Itsuki Sakon. The Asymmetric Thermal Emission of Protoplanetary Disk Surrounding HD 142527 Seen by Subaru/COMICS
  9. ^ Simon Casassus et al. Flows of gas through a protoplanetary gap. Nature (02 January 2013).
  10. ^ Simon Casassus et al. ,Flows of gas through a protoplanetary gap, Nature 493, 191–194 (10 January 2013).
  11. ^ Honda, M.; Inoue, A. K.; Fukagawa, M.; Oka, A.; Nakamoto, T.; Ishii, M.; Terada, H.; Takato, N.; Kawakita, H.; Okamoto, Y. K.; Shibai, H.; Tamura, M.; Kudo, T.; Itoh, Y. Detection of Water Ice Grains on the Surface of the Circumstellar Disk Around HD 142527. The Astrophysical Journal Letters, Volume 690, Issue 2, pp. L110-L113 (2009).
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