75 Ceti: Difference between revisions
Content deleted Content added
Praemonitus (talk | contribs) Ref. data update |
m add url for ref |
||
| Line 74: | Line 74: | ||
| bibcode=2007MNRAS.382..553L | doi=10.1111/j.1365-2966.2007.11852.x }}</ref> |
| bibcode=2007MNRAS.382..553L | doi=10.1111/j.1365-2966.2007.11852.x }}</ref> |
||
<ref name="Sato2012">{{cite journal | title=Substellar Companions to Seven Evolved Intermediate-Mass Stars | last1=Sato | first1=Bun'ei | last2=Omiya | first2=Masashi | last3=Harakawa | first3=Hiroki | last4=Izumiura | first4=Hideyuki | last5=Kambe | first5=Eiji | last6=Takeda | first6=Yoichi | last7=Yoshida | first7=Michitoshi | last8=Itoh | first8=Yoichi | last9=Ando | first9=Hiroyasu | last10=Kokubo | first10=Eiichiro | last11=Ida | first11=Shigeru | display-authors=1 | journal=Publications of the Astronomical Society of Japan | volume=64 | issue=6 | at=135 | |
<ref name="Sato2012">{{cite journal | title=Substellar Companions to Seven Evolved Intermediate-Mass Stars | url=https://academic.oup.com/pasj/article/64/6/135/1422181 | last1=Sato | first1=Bun'ei | last2=Omiya | first2=Masashi | last3=Harakawa | first3=Hiroki | last4=Izumiura | first4=Hideyuki | last5=Kambe | first5=Eiji | last6=Takeda | first6=Yoichi | last7=Yoshida | first7=Michitoshi | last8=Itoh | first8=Yoichi | last9=Ando | first9=Hiroyasu | last10=Kokubo | first10=Eiichiro | last11=Ida | first11=Shigeru | display-authors=1 | journal=Publications of the Astronomical Society of Japan | volume=64 | issue=6 | at=135 | year=2012 | arxiv=1207.3141 | bibcode=2012PASJ...64..135S | doi=10.1093/pasj/64.6.135 }}</ref> |
||
<ref name="van Leeuwen2007">{{cite journal | title=Validation of the new Hipparcos reduction | url=http://www.aanda.org/articles/aa/full/2007/41/aa8357-07/aa8357-07.html | last1=van Leeuwen | first1=F. | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | date=2007 | arxiv=0708.1752 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 }}[http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/311/hip2&recno=11763 Vizier catalog entry ]</ref> |
<ref name="van Leeuwen2007">{{cite journal | title=Validation of the new Hipparcos reduction | url=http://www.aanda.org/articles/aa/full/2007/41/aa8357-07/aa8357-07.html | last1=van Leeuwen | first1=F. | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | date=2007 | arxiv=0708.1752 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 }}[http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/311/hip2&recno=11763 Vizier catalog entry ]</ref> |
||
Revision as of 20:55, 2 March 2018
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cetus |
| Right ascension | 02h 32m 09.422s[1] |
| Declination | −01° 02′ 05.62″[1] |
| Apparent magnitude (V) | +5.36 |
| Characteristics | |
| Spectral type | G3 III |
| Astrometry | |
| Proper motion (μ) | RA: -24.72 ± 0.46[1] mas/yr Dec.: -32.08 ± 0.40[1] mas/yr |
| Parallax (π) | 12.28 ± 0.45 mas[1] |
| Distance | 266 ± 10 ly (81 ± 3 pc) |
| Absolute magnitude (MV) | 0.808[2] |
| Details | |
| Mass | 2.16[2] M☉ |
| Radius | 10.5 (9.5–11.5) R☉ |
| Luminosity | 53.7 L☉ |
| Surface gravity (log g) | 2.75[2] cgs |
| Temperature | 4,784[2] K |
| Metallicity | −0.05[2] |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
75 Ceti is a G-type giant with at least one planet.[3]
In Chinese, 天囷 (Tiān Qūn), meaning Circular Celestial Granary, refers to an asterism consisting of α Ceti, κ1 Ceti, λ Ceti, μ Ceti, ξ1 Ceti, ξ2 Ceti, ν Ceti, γ Ceti, δ Ceti, 75 Ceti, 70 Ceti, 63 Ceti and 66 Ceti. Consequently, 75 Ceti itself is known as the Tenth Star of Circular Celestial Granary.[4]
The planet's discoverers consider this planet b "typical" of gas giants.[3] Note that (like many recorded planets) b takes in much more insolation than does Jupiter and, indeed, Earth.[5]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >3 MJ | 2.1 | 691.9 ± 3.6 | 0.117 ± 0.048 | — | — |
There may be additional periodic factors in the data, corresponding to m sin i of around 0.4 MJ and 1 MJ, at distances of ∼0.9 AU and ∼4 AU. If these are confirmed, they are more irradiated than Earth as well.
References
- ^ a b c d e van Leeuwen, F. (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.Vizier catalog entry
- ^ a b c d e Liu, Y. J.; et al. (2007), "The abundances of nearby red clump giants", Monthly Notices of the Royal Astronomical Society, 382 (2): 553–66, Bibcode:2007MNRAS.382..553L, doi:10.1111/j.1365-2966.2007.11852.x.
- ^ a b c Sato, Bun'ei; et al. (2012). "Substellar Companions to Seven Evolved Intermediate-Mass Stars". Publications of the Astronomical Society of Japan. 64 (6). 135. arXiv:1207.3141. Bibcode:2012PASJ...64..135S. doi:10.1093/pasj/64.6.135.
- ^ Template:Zh icon AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
- ^ Square root of luminosity means that an Earth like planet would have to be >7 AU from the star.
 | This giant-star-related article is a stub. You can help Wikipedia by expanding it. |