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| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h 41m 25.34114s[1] |
| Declination | +48° 45′ 14.9900″[1] |
| Apparent magnitude (V) | 13.12[2] |
| Characteristics | |
| Evolutionary stage | main sequence[1] |
| Spectral type | F7V[3] |
| B−V color index | +0.33[2] |
| Variable type | δ Scuti[4] |
| Astrometry | |
| Radial velocity (Rv) | −136±4[5] km/s |
| Proper motion (μ) | RA: −20.900 mas/yr[1] Dec.: −3.693 mas/yr[1] |
| Parallax (π) | 0.8344 ± 0.01 mas[1] |
| Distance | 3,910 ± 50 ly (1,200 ± 10 pc) |
| Details | |
| Mass | 1.46[6] M☉ |
| Radius | 1.57±0.07[7] R☉ |
| Luminosity | 12.6[8] L☉ |
| Surface gravity (log g) | 4.22[8] cgs |
| Temperature | 7,590[8] K |
| Metallicity [Fe/H] | −0.1±0.11[8] dex |
| Rotation | ≈100 days[8] |
| Rotational velocity (v sin i) | 1[8] km/s |
| Age | 756[1] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
KIC 11145123 (sometimes mistakenly called Kepler 11145123[9]), is a white hued star located in the northern constellation Cygnus, the swan. It has an apparent magnitude of 13.12,[2] making it readily visible in large telescopes, but not to the naked eye. The object is located relatively far at a distance of approximately 3,910 light years,[1] but is rapidly approaching the Solar System with a radial velocity of −136 km/s.[5]
Characteristics
[edit]KIC 11145123 has a spectral classification of F7V,[3] indicating that it is a main sequence F-type star. Atmospheric models suggest it may be hotter and possibly a late A-type star.[4] It has 1.4 times the mass of the Sun, in contrast to the 1.7 times that would be expected from a normal late A main sequence star, and 1.57 times its radius.[7] It radiates 12 times the luminosity of the Sun from its photosphere at an effective temperature of 7,590 K.[8] Unlike most hot stars, KIC 11145123 spins exceptionally slowly with a projected rotational velocity of 1 km/s.[8] This corresponds to a period of roughly 100 days.[8] Despite appearing as a main sequence star (Gaia DR3 models it as such),[1] it is most likely a blue straggler.[10][6]
Roundest natural object
[edit]KIC 11145123 is currently believed be the roundest natural object, with the difference between equatorial and polar radii equaling a mere three kilometers.[9]
References
[edit]- ^ a b c d e f g h 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 Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (2012). "VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012)". VizieR On-line Data Catalog: I/322A. Originally Published in: 2012yCat.1322....0Z; 2013AJ....145...44Z. 1322. Bibcode:2012yCat.1322....0Z.
- ^ a b Frasca, A.; Molenda-Żakowicz, J.; De Cat, P.; Catanzaro, G.; Fu, J. N.; Ren, A. B.; Luo, A. L.; Shi, J. R.; Wu, Y.; Zhang, H. T. (2016). "Activity indicators and stellar parameters of the Kepler targets. An application of the ROTFIT pipeline to LAMOST-Kepler stellar spectra". Astronomy and Astrophysics. 594. arXiv:1606.09149. Bibcode:2016A&A...594A..39F. doi:10.1051/0004-6361/201628337. S2CID 119283349.
- ^ a b Kurtz, Donald W.; Saio, Hideyuki; Takata, Masao; Shibahashi, Hiromoto; Murphy, Simon J.; Sekii, Takashi (13 August 2014). "Asteroseismic measurement of surface-to-core rotation in a main-sequence A star, KIC 11145123". Monthly Notices of the Royal Astronomical Society. 444 (1): 102–116. arXiv:1405.0155. Bibcode:2014MNRAS.444..102K. doi:10.1093/mnras/stu1329. eISSN 1365-2966. ISSN 0035-8711.
- ^ a b Tsantaki, M.; Pancino, E.; Marrese, P.; Marinoni, S.; Rainer, M.; Sanna, N.; Turchi, A.; Randich, S.; Gallart, C.; Battaglia, G.; Masseron, T. (March 2022). "Survey of Surveys". Astronomy & Astrophysics. 659: A95. arXiv:2110.09316. Bibcode:2022A&A...659A..95T. doi:10.1051/0004-6361/202141702. eISSN 1432-0746. ISSN 0004-6361.
- ^ a b Hatta, Yoshiki; Sekii, Takashi; Takata, Masao; Benomar, Othman (2021). "Nonstandard Modeling of a Possible Blue Straggler Star, KIC 11145123". The Astrophysical Journal. 923 (2): 244. arXiv:2110.06926. Bibcode:2021ApJ...923..244H. doi:10.3847/1538-4357/ac23c9. S2CID 238856685.
- ^ a b Stassun, Keivan G.; et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. eISSN 1538-3881.
- ^ a b c d e f g h i Takada-Hidai, Masahide; Kurtz, Donald W.; Shibahashi, Hiromoto; Murphy, Simon J.; Takata, Masao; Saio, Hideyuki; Sekii, Takashi (2017). "Spectroscopic and asteroseismic analysis of the remarkable main-sequence a star KIC 11145123". Monthly Notices of the Royal Astronomical Society. 470 (4): 4908. arXiv:1706.04314. Bibcode:2017MNRAS.470.4908T. doi:10.1093/mnras/stx1506.
- ^ a b "Kepler 11145123 is Most Spherical Natural Object Ever Seen, Astronomers Say | Astronomy | Sci-News.com". Breaking Science News | Sci-News.com. 18 November 2016. Retrieved 2021-04-26.
- ^ Hatta, Yoshiki; Sekii, Takashi; Takata, Masao; Kurtz, Donald W. (2019). "The Two-dimensional Internal Rotation of KIC 11145123". The Astrophysical Journal. 871 (2): 135. arXiv:2111.06853. Bibcode:2019ApJ...871..135H. doi:10.3847/1538-4357/aaf881. S2CID 127611459.