Astronomy:HD 142527
250px Artist’s impression of the disc and gas streams around HD 142527 | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Lupus[1] |
| Right ascension | 15h 56m 41.88986s[2] |
| Declination | −42° 19′ 23.2746″[2] |
| Apparent magnitude (V) | 8.34[3] |
| Characteristics | |
| Spectral type | F6 III[3] |
| Astrometry | |
| Radial velocity (Rv) | -3.10[3] km/s |
| Proper motion (μ) | RA: -11.19[2] mas/yr Dec.: -24.46[2] mas/yr |
| Parallax (π) | 6.2791 ± 0.0284[4] mas |
| Distance | 519 ± 2 ly (159.3 ± 0.7 pc) |
| Details | |
| HD 142527 A | |
| Mass | 2.2±0.05[5] M☉ |
| Radius | 3.46±0.13[5] R☉ |
| Luminosity | 22.39±0.52[5] L☉ |
| Surface gravity (log g) | 3.15[6] cgs |
| Temperature | 6632[6] K |
| Metallicity [Fe/H] | 0.33[6] dex |
| Age | 4.4+0.49−0.38[5] Myr |
| HD 142527 B | |
| Mass | 0.34±0.06[7] M☉ |
| Radius | 1.37±0.05[7] R☉ |
| Luminosity | 0.25±0.04[7] L☉ |
| Temperature | 3500±100[7] K |
| Age | 1.8+1.2−-0.5[7] Myr |
| Orbit[8] | |
| Primary | HD 142527 A |
| Companion | HD 142527 B |
| Period (P) | 23.50±0.85 yr |
| Semi-major axis (a) | 0.0678±0.014" (10.80±0.22 AU) |
| Eccentricity (e) | 0.47±0.01 |
| Inclination (i) | 149.47±0.71° |
| Longitude of the node (Ω) | 161.51±2.01° |
| Periastron epoch (T) | 2020.42±0.05 |
| Argument of periastron (ω) (secondary) | 186.45±0.48° |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 142527 is a binary star system in the constellation of Lupus.[10][11] 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[12] with a projected separation of less than 0.1″.[13] 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.[12]
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.[14]
Protoplanetary disk
HD 142527 is an extremely young star system, aged about 4.4 million years old[5] 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.[11] 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.[11] 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[15] 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
- ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific 99 (617): 695. doi:10.1086/132034. Bibcode: 1987PASP...99..695R Constellation record for this object at VizieR.
- ↑ 2.0 2.1 2.2 2.3 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. Vizier catalog entry
- ↑ 3.0 3.1 3.2 3.3 "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.
- ↑ 5.0 5.1 5.2 5.3 5.4 Guzmán-Díaz, J.; Mendigutía, I.; Montesinos, B.; Oudmaijer, R. D.; Vioque, M.; Rodrigo, C.; Solano, E.; Meeus, G. et al. (2021). "Homogeneous study of Herbig Ae/Be stars from spectral energy distributions and Gaia EDR3". Astronomy & Astrophysics 650: A182. doi:10.1051/0004-6361/202039519. Bibcode: 2021A&A...650A.182G.
- ↑ 6.0 6.1 6.2 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.
- ↑ 7.0 7.1 7.2 7.3 7.4 Christiaens, V.; Casassus, S.; Absil, O.; Kimeswenger, S.; Gomez Gonzalez, C. A.; Girard, J.; Ramírez, R.; Wertz, O. et al. (2018). "Characterization of low-mass companion HD 142527 B". Astronomy & Astrophysics 617: A37. doi:10.1051/0004-6361/201629454. Bibcode: 2018A&A...617A..37C.
- ↑ Nowak, M.; Rowther, S.; Lacour, S.; Meru, F.; Nealon, R.; Price, D. J. (2024). "The orbit of HD 142527 B is too compact to explain many of the disc features". Astronomy & Astrophysics 683: A6. doi:10.1051/0004-6361/202347748. Bibcode: 2024A&A...683A...6N.
- ↑ "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.
- ↑ 11.0 11.1 11.2 Casassus, Simon; Van Der Plas, Gerrit M.; Perez, Sebastian; Dent, William R. F.; Fomalont, Ed; Hagelberg, Janis; Hales, Antonio; Jordán, Andrés et al. (2013). "Flows of gas through a protoplanetary gap". Nature 493 (7431): 191–194. doi:10.1038/nature11769. PMID 23283173. Bibcode: 2013Natur.493..191C.
- ↑ 12.0 12.1 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.
- ↑ 13.0 13.1 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.
- ↑ Honda, M.; Inoue, A. K.; Fukagawa, M.; Oka, A.; Nakamoto, T.; Ishii, M.; Terada, H.; Takato, N. et al. (2009). "Detection of Water Ice Grains on the Surface of the Circumstellar Disk Around HD 142527". The Astrophysical Journal 690 (2): L110–L113. doi:10.1088/0004-637X/690/2/L110. Bibcode: 2009ApJ...690L.110H.
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