User:AluminiumWithAnI/Kepler-1972
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lyra |
| Right ascension | 19h 13m 34.86914s[1] |
| Declination | 39° 52′ 21.4698″[1] |
| Characteristics | |
| Spectral type | G[2] |
| Astrometry | |
| Radial velocity (Rv) | 5.04±0.54[1] km/s |
| Proper motion (μ) | RA: 3.441 mas/yr[1] Dec.: −28.778 mas/yr[1] |
| Parallax (π) | 3.5329 ± 0.0107 mas[1] |
| Distance | 923 ± 3 ly (283.1 ± 0.9 pc) |
| Absolute magnitude (MV) | [3] |
| Details | |
| Mass | 1.12±0.03 M☉ |
| Radius | 1.384±0.050 R☉ |
| Luminosity (bolometric) | 1.97±0.07 L☉ |
| Surface gravity (log g) | 4.20±0.04 cgs |
| Temperature | 5818±50 K |
| Metallicity [Fe/H] | 0.23±0.01 dex |
| Age | 7.4 ± 1.2 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Kepler-1972 (KOI-3184) is a solitary G-type star in the northern constellation of Lyra, some 923 light-years (283 pc) distant. It is similar in temperature to the Sun, but 12% more massive, 38.4% larger and roughly twice as bright. It is host to two confirmed exoplanets and a third planet is suspected.[5] It is located at the celestial coordinates: right ascension 19h 13m 34.9s, declination +39° 52′ 21.5″.[1]
Position
[edit]Kepler-1972 is located in the western portion of constellation Lyra, placing it near the southern edge of Kepler's field of view. It is situated 10.6″ west of and 43′36″ north of Eta Lyrae (η Lyrae; Aladfar), a 4th-magnitude B-type subgiant[6] 10 times more massive than the Sun and 19,000 times more luminous,[7] at 1,390 light-years (430 pc) away,[8] which is part of a spectroscopic binary[9] and an optical double.[10]
Stellar characteristics
[edit]| Sun | Kepler-1972 |
|---|---|
|
|
Kepler-1972 is a G-type star at the end of its main sequence lifespan.
It has an apparent magnitude of 11.2,[4] making it too dim to be seen from Earth by the naked eye,[11] but observable using a 35 mm aperture telescope.[12]
Planetary system
[edit]| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| .03 (unconfirmed) | — | — | 4.020184 ± 0.000035 | — | 87.25 +1.31 −0.97° |
0.551 ± 0.034 R🜨 |
| b | 2.02 +0.56 −0.62 M🜨 |
— | 7.54425 ± 0.00054 | 0.067 +0.071 −0.040 |
87.62 +0.73 −0.49° |
0.802 +0.042 −0.041 R🜨 |
| c | 2.11 +0.59 −0.65 M🜨 |
— | 11.3295 ± 0.0011 | 0.043 +0.046 −0.028 |
87.13 +0.17 −0.19° |
0.868 +0.051 −0.050 R🜨 |
Kepler-1972 is host to two confirmed planets and at least one additional planetary candidate. All three planets are smaller than Earth.
Size comparison
[edit]The chart below shows an approximate size comparison between the three planets around Kepler-1972 (two confirmed, one candidate), alongside Earth (6371.0 km; 1 R🜨)[14] and Mars (3,398.5 km;[15] 0.533 R🜨) for reference.
| Mars | KOI-3184.03 | Kepler-1972b | Kepler-1972c | Earth |
|---|---|---|---|---|
 |
|
|
|
 |
See also
[edit]References
[edit]- ^ a b c d e f 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. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ Cite error: The named reference
Escude2012was invoked but never defined (see the help page). - ^ Cite error: The named reference
Holmberg2009was invoked but never defined (see the help page). - ^ a b "Kepler-1972". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2024-05-24.
- ^ Leleu, A.; Delisle, J. -B.; Mardling, R.; Udry, S.; Chatel, G.; Alibert, Y.; Eggenberger, P. (2022), "Alleviating the transit timing variation bias in transit surveys", Astronomy & Astrophysics, 661: A141, arXiv:2201.11459, doi:10.1051/0004-6361/202142822, S2CID 246294682
- ^ "eta Lyr". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2024-05-24.
- ^ Hohle, M. M.; et al. (April 2010). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten. 331 (4): 349. arXiv:1003.2335. Bibcode:2010AN....331..349H. doi:10.1002/asna.200911355. S2CID 111387483.
- ^ van Leeuwen, F. (November 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.
- ^ Abt, H. A.; Levy, S. G. (1978). "Binaries among B2-B5 IV, V absorption and emission stars". The Astrophysical Journal Supplement Series. 36: 241. Bibcode:1978ApJS...36..241A. doi:10.1086/190498.
- ^ Mason, B. D.; et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
- ^ John E. Bortle (February 2001). "The Bortle Dark-Sky Scale". Sky & Telescope. Archived from the original on 2009-03-23. Retrieved 2009-11-18.
- ^ North, Gerald; James, Nick (2014). Observing Variable Stars, Novae and Supernovae. Cambridge University Press. p. 24. ISBN 978-1-107-63612-5.
- ^ Cite error: The named reference
arxivwas invoked but never defined (see the help page). - ^ Various (2000). David R. Lide (ed.). Handbook of Chemistry and Physics (81st ed.). CRC Press. ISBN 978-0-8493-0481-1.
- ^ Seidelmann, P. Kenneth; et al. (2007). "Report of the IAU/IAG Working Group on cartographic coordinates and rotational elements: 2006". Celestial Mechanics and Dynamical Astronomy. 98 (3): 155–180. Bibcode:2007CeMDA..98..155S. doi:10.1007/s10569-007-9072-y.