Astronomy:HD 142527
 Artist’s impression of the disc and gas streams around HD 142527 | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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 |
| Distance | 519 ± 2 ly (159.3 ± 0.7 pc) |
| Details | |
| Mass | 2.5 M☉ |
| Surface gravity (log g) | 3.15[4] cgs |
| Temperature | 6632[4] K |
| Metallicity [Fe/H] | 0.33[4] dex |
| Age | 1 Myr |
| Orbit[5] | |
| Primary | HD 142527 A |
| Companion | HD 142527 B |
| Semi-major axis (a) | 14.71+8.18−2.33 AU |
| Eccentricity (e) | 0.28+0.22−0.10 |
| Inclination (i) | 126.27+2.13−2.28° |
| Longitude of the node (Ω) | 142.38+5.51−6.12° |
| Periastron epoch (T) | 2021.07+0.82−0.72 |
| Argument of periastron (ω) (secondary) | 86.02+52.31−42.59° |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 142527 is a binary star system in the constellation of Lupus.[7][8] The primary star belongs to the Herbig Ae/Be star class, while the companion, discovered in 2012, is a red dwarf star or accreting protoplanet[5] with a projected separation of less than 0.1″.[9] The system is notable for its circumbinary protoplanetary disk and its discovery has helped refine models of planet formation. The orbit of companion is strongly inclined to the circumbinary protoplanetary disk.[5]
HD 142527 is listed in the International Variable star index as a UX Orionis variable, with a visible-light magnitude ranging from 8.27 to 8.60.[10]
Protoplanetary disk
HD 142527 is an extremely young star system, aged about 1 million years old[11] so it retains its protoplanetary disk, which has a mass of 15% 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.[12] 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.[13] 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.
Japan ese astronomers have discovered particles of ice[14] in the disk.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| protoplanetary disk | 140–550 AU | 28° | — | |||
References
- ↑ 1.0 1.1 1.2 1.3 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL. Vizier catalog entry
- ↑ 2.0 2.1 2.2 2.3 "HD 142527". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+142527.
- ↑ Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 4.0 4.1 4.2 Luck, R. Earle (2015). "Abundances in the Local Region. I. G and K Giants". The Astronomical Journal 150 (3): 88. doi:10.1088/0004-6256/150/3/88. Bibcode: 2015AJ....150...88L.
- ↑ 5.0 5.1 5.2 Balmer, William O.; Follette, Katherine B.; Close, Laird M.; Males, Jared R.; De Rosa, Robert J.; Adams Redai, Jéa I.; Watson, Alex; Weinberger, Alycia J. et al. (2022). "Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B". The Astronomical Journal 164 (1): 29. doi:10.3847/1538-3881/ac73f4. Bibcode: 2022AJ....164...29B.
- ↑ "ASAS-SN Variable Stars Database". ASAS-SN. https://asas-sn.osu.edu/variables/lookup.
- ↑ "Hd 142527". http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+142527.
- ↑ 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) .
- ↑ 9.0 9.1 Hunziker, S.; Schmid, H. M.; Ma, J.; Menard, F.; Avenhaus, H.; Boccaletti, A.; Beuzit, J. L.; Chauvin, G. et al. (2021), "HD 142527: Quantitative disk polarimetry with SPHERE", Astronomy & Astrophysics 648: A110, doi:10.1051/0004-6361/202040166, Bibcode: 2021A&A...648A.110H
- ↑ "NSV 20441". AAVSO. https://www.aavso.org/vsx/index.php?view=detail.top&oid=58876.
- ↑ 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
- ↑ Simon Casassus et al. Flows of gas through a protoplanetary gap. Nature (02 January 2013).
- ↑ Simon Casassus et al. ,Flows of gas through a protoplanetary gap, Nature 493, 191–194 (10 January 2013).
- ↑ 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).
 |  |
