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HD 142
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Phoenix[1] |
| HD 142 A | |
| Right ascension | 00h 06m 19.1754s[2] |
| Declination | −49° 04′ 30.6741″[2] |
| Apparent magnitude (V) | 5.711±0.003[3] |
| HD 142 B | |
| Right ascension | 00h 06m 19.1480s[4] |
| Declination | −49° 04′ 34.9177″[4] |
| Apparent magnitude (V) | +11.5[5] |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | F7V[6] + K8.5-M1.5[7] |
| B−V color index | 0.519±0.011[8] |
| Astrometry | |
| HD 142 A | |
| Radial velocity (Rv) | 5.76±0.12[9] km/s |
| Proper motion (μ) | RA: 575.099[9] mas/yr Dec.: −40.874[9] mas/yr |
| Parallax (π) | 38.1945±0.0355 mas[9] |
| Distance | 85.39 ± 0.08 ly (26.18 ± 0.02 pc) |
| Absolute magnitude (MV) | 3.66±0.02[10] |
| HD 142 B | |
| Proper motion (μ) | RA: 566.984[11] mas/yr Dec.: −17.387[11] mas/yr |
| Parallax (π) | 38.2306±0.0349 mas[11] |
| Distance | 85.31 ± 0.08 ly (26.16 ± 0.02 pc) |
| Details | |
| HD 142 A | |
| Mass | 1.25±0.01[12] M☉ |
| Radius | 1.41±0.11[13] R☉ |
| Luminosity | 2.9[13] L☉ |
| Surface gravity (log g) | 4.45±0.07[12] cgs |
| Temperature | 6,349±26[12] K |
| Metallicity [Fe/H] | +0.133±0.020[12] dex |
| Rotation | 27.15 days[14] |
| Rotational velocity (v sin i) | 9.58±0.74[15] km/s |
| Age | 2.50+0.32 −0.28[12] Gyr |
| HD 142 B | |
| Mass | 0.643[16] M☉ |
| Radius | 0.423[16] R☉ |
| Luminosity | 0.046[16] L☉ |
| Surface gravity (log g) | 4.99[16] cgs |
| Temperature | 4,110[16] K |
| Other designations | |
| HD 142A: CD−49°14337, HD 142, HIP 522, HR 6, SAO 214963, WDS J00063-4905A[17] | |
| HD 142B: CD−49°14337B, WDS J00063-4905B, NLTT 218, 2MASS J00061919-4904348[18] | |
| Database references | |
| SIMBAD | data |
| B | |
HD 142 is a wide binary star[5] system in the southern constellation of Phoenix. The main component has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.7.[3] The system is located at a distance of 85.5 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +6 km/s.[19]
The primary component is an F-type main-sequence star with a stellar classification of F7V,[6] which indicates it is undergoing core hydrogen fusion. It is an estimated 2.5 billion years old[12] and is spinning with a projected rotational velocity of 10 km/s.[15] The star has 1.25 times the mass of the Sun[12] and 1.4 times the Sun's radius. It is radiating 2.9 times the luminosity of the Sun from its photosphere[13] at an effective temperature of 6,349 K.[12]
A magnitude 11.5[5] companion star was detected in 1894 making this a binary star system.[20] The binary companion was confirmed to be gravitationally bound in 2007 and determined to be a red dwarf of spectral type K8.5-M1.5[7] with 54% of the Sun's mass.[21] The pair have a projected separation of 120.6 AU.[21]
Planetary system
[edit]In 2001, the Anglo-Australian Planet Search team led by Chris Tinney announced the discovery of an extrasolar planet orbiting the primary star.[22][23] An additional linear trend in the radial velocity data was noticed in 2006[24] that could have been due to another planet or to the stellar companion.[25] In 2012, additional measurements allowed the detection of a second planet. A third possible planet with a period of 108 days was seen in the data, but with a false alarm probability of five percent.[26] Another paper by the same team updated the parameters for b and c but did not mention the possible planet d.[27]
An astrometric measurement of HD 142 b's inclination and true mass was published in 2022 as part of Gaia DR3.[28] Another 2022 study determined the inclination and true mass of planet c, and confirmed the existence of planet d.[29]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| d | ≥0.260+0.032 −0.036 MJ |
0.474+0.021 −0.023 |
108.5±0.1 | 0.130+0.103 −0.085 |
— | — |
| b | 7.1±1.0 MJ | 1.039+0.046 −0.051 |
351.4±0.4 | 0.158+0.033 −0.030 |
59±7° | — |
| c | 10.901+1.278 −0.937 MJ |
9.811+0.515 −0.520 |
10,159.6+384.8 −321.9 |
0.277+0.026 −0.027 |
90.374+10.495 −12.319° |
— |
See also
[edit]References
[edit]- ^ Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Vizier query form
- ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b Olsen, E. H. (1994). "Stroemgren photometry of F- and G-type stars brighter than V = 9.6. I. UVBY photometry". Astronomy and Astrophysics Supplement Series. 106: 257–266. Bibcode:1994A&AS..106..257O. Vizier catalog entry
- ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c Eggleton, P. P.; Tokovinin, A.A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x.
- ^ a b Gray, R. O.; et al. (2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc - The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637.
- ^ a b Eggenberger, A.; et al. (2007). "The impact of stellar duplicity on planet occurrence and properties I. Observational results of a VLT/NACO search for stellar companions to 130 nearby stars with and without planets". Astronomy and Astrophysics. 474 (1): 273–291. Bibcode:2007A&A...474..273E. doi:10.1051/0004-6361:20077447.
- ^ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b c d 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.
- ^ Holmberg; et al. (2009). "HD 142". Geneva-Copenhagen Survey of Solar neighbourhood III. Retrieved 2010-01-27.
- ^ a b c 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.
- ^ a b c d e f g h Carvalho-Silva, Gabriela; Meléndez, Jorge; Rathsam, Anne; Shejeelammal, J.; Martos, Giulia; Lorenzo-Oliveira, Diego; Spina, Lorenzo; Ribeiro Alves, Débora (April 2025). "A New Age–Activity Relation For Solar Analogs that Accounts for Metallicity". The Astrophysical Journal Letters. 983 (2): L31. arXiv:2504.17482. Bibcode:2025ApJ...983L..31C. doi:10.3847/2041-8213/adc382. ISSN 2041-8205.
- ^ a b c Ghezzi, L.; et al. (September 2010). "Stellar Parameters and Metallicities of Stars Hosting Jovian and Neptunian Mass Planets: A Possible Dependence of Planetary Mass on Metallicity". The Astrophysical Journal. 720 (2): 1290–1302. arXiv:1007.2681. Bibcode:2010ApJ...720.1290G. doi:10.1088/0004-637X/720/2/1290.
- ^ Oelkers, Ryan J.; Rodriguez, Joseph E.; Stassun, Keivan G.; Pepper, Joshua; Somers, Garrett; Kafka, Stella; Stevens, Daniel J.; Beatty, Thomas G.; Siverd, Robert J.; Lund, Michael B.; Kuhn, Rudolf B.; James, David; Gaudi, B. Scott (2018). "Variability Properties of Four Million Sources in the TESS Input Catalog Observed with the Kilodegree Extremely Little Telescope Survey". The Astronomical Journal. 155 (1): 39. arXiv:1711.03608. Bibcode:2018AJ....155...39O. doi:10.3847/1538-3881/aa9bf4.
- ^ a b Soto, M. G.; Jenkins, J. S. (July 2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy & Astrophysics. 615: 28. arXiv:1801.09698. Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533. A76.
- ^ a b c d e Tuchow, Noah W.; Stark, Christopher C.; Mamajek, Eric (2024). "HPIC: The Habitable Worlds Observatory Preliminary Input Catalog". The Astronomical Journal. 167 (3): 139. Bibcode:2024AJ....167..139T. doi:10.3847/1538-3881/ad25ec.
- ^ "HD 142". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-08-12.
- ^ "HD 142B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-08-12.
- ^ Valenti, J. A.; Fischer, D. A. (2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". The Astrophysical Journal Supplement Series. 159 (1): 141–166. Bibcode:2005ApJS..159..141V. doi:10.1086/430500.
- ^ Raghavan, Deepak; et al. (2006). "Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems". The Astrophysical Journal. 646 (1): 523–542. arXiv:astro-ph/0603836. Bibcode:2006ApJ...646..523R. doi:10.1086/504823.
- ^ a b Tokovinin, A.; Kiyaeva, O. (February 2016). "Eccentricity distribution of wide binaries". Monthly Notices of the Royal Astronomical Society. 456 (2): 2070–2079. arXiv:1512.00278. Bibcode:2016MNRAS.456.2070T. doi:10.1093/mnras/stv2825.
- ^ "Astronomers close in on Solar System's 'siblings'" (Press release). Marsfield, New South Wales, Australia: Australian Astronomical Observatory. October 15, 2001. Archived from the original on August 22, 2016. Retrieved July 10, 2016.
- ^ Tinney, C. G.; et al. (2002). "Two Extrasolar Planets from the Anglo-Australian Planet Search". The Astrophysical Journal. 571 (1): 528–531. arXiv:astro-ph/0111255. Bibcode:2002ApJ...571..528T. doi:10.1086/339916.
- ^ Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701.
- ^ Wright, J. T.; et al. (2007). "Four New Exoplanets and Hints of Additional Substellar Companions to Exoplanet Host Stars". The Astrophysical Journal. 657 (1): 533–545. arXiv:astro-ph/0611658. Bibcode:2007ApJ...657..533W. doi:10.1086/510553.
- ^ Wittenmyer, Robert A.; et al. (2012). "The Anglo-Australian Planet Search. XXII. Two New Multi-planet Systems". The Astrophysical Journal. 753 (2). 169. arXiv:1205.2765. Bibcode:2012ApJ...753..169W. doi:10.1088/0004-637X/753/2/169.
- ^ Wittenmyer, Robert A.; et al. (2020). "Cool Jupiters greatly outnumber their toasty siblings: occurrence rates from the Anglo-Australian Planet Search". Monthly Notices of the Royal Astronomical Society. 492 (1): 377–383. arXiv:1912.01821. Bibcode:2020MNRAS.492..377W. doi:10.1093/mnras/stz3436.
- ^ a b Gaia Collaboration; et al. (2023). "Gaia Data Release 3". Astronomy & Astrophysics. 674: A34. arXiv:2206.05595. Bibcode:2023A&A...674A..34G. doi:10.1051/0004-6361/202243782. S2CID 249626026.
- ^ a b Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21): 21. arXiv:2208.12720. Bibcode:2022ApJS..262...21F. doi:10.3847/1538-4365/ac7e57. S2CID 251864022.
External links
[edit]- "HD 142". Open Exoplanet Catalogue. Retrieved 2014-09-08.
