75 Ceti

{{Starbox observe

| epoch = J2000.0

| constell = Cetus

| ra = {{RA|02|32|09.42241}}

| dec = {{DEC|-01|02|05.6166}}

| appmag_v = +5.36

}}

{{Starbox character

| type = red clump

| class = K1 III or G3 III

| b-v = {{Val|+1.004|0.002}}

| variable =

}}

{{Starbox astrometry

| radial_v = {{val|−6.34|0.13}}

| prop_mo_ra = −23.268

| prop_mo_dec = −30.987

| pm_footnote =

| parallax = 12.1717

| p_error = 0.0962

| parallax_footnote =

| absmag_v = 0.808

}}

{{Starbox detail

| mass = {{Val|1.92|0.07|0.08}}

| radius = {{val|10.57|0.17|0.16}}

| luminosity = {{Val|51.8|1.5|2.5}}

| temperature = {{Val|4830|20|fmt=commas}}

| gravity = {{Val|2.67|0.04}}

| metal_fe = {{Val|+0.10|0.08|0.05}}

| rotational_velocity = {{val|3.2|0.5}}

| age_gyr = {{Val|1.41|0.01}}

}}

{{Starbox catalog

| names = {{odlist | F=75 Cet | BD=−01°353 | GC=3043 | HD=15779 | HIP=11791 | HR=739 | SAO=129959 }}

}}

{{Starbox reference

| Simbad = 75+Cet

| NSTED = 75%20Cet

| EPE = 75+Cet

}}

75 Ceti is a star in the equatorial constellation of Cetus with at least two planets. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of +5.36. The star is located {{convert|268|ly|pc|lk=on|abbr=off}} distant from the Sun, based on parallax, but is drifting closer with a radial velocity of −6 km/s.

In Chinese, {{lang|zh|天囷}} ({{lang|zh-Latn|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.{{in lang|zh}} [http://aeea.nmns.edu.tw/2006/0607/ap060711.html AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日] {{Webarchive|url=https://web.archive.org/web/20120204114123/http://aeea.nmns.edu.tw/2006/0607/ap060711.html |date=2012-02-04 }}

This is an aging giant star with a stellar classification of K1 III, having exhausted the supply of hydrogen at its core and expanded to 10.6 times the Sun's radius, or {{Convert|10.6|solar radius|AU|2|disp=out|lk=on}}. It is a red clump giant, which indicates it is on the horizontal branch and is generating energy through helium fusion at the core. The star is 1.4 billion years old with 1.9 times the Sun's mass. It is radiating 56 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,846 K. There is a companion star just over half the Sun's mass at a separation of 11.5 arcseconds, corresponding to 958 AU.

Planetary system

A planetary companion was discovered by Doppler measurements at the Okayama Astrophysical Observatory, and announced in 2012. The planet's discoverers consider the planet, designated 75 Ceti b, to be "typical" of gas giants. Note that (like many recorded planets) b takes in much more insolation than does Jupiter and, indeed, Earth.Square root of luminosity means that an Earth like planet would have to be >7 AU from the star.

There may be additional periodic factors in the data, corresponding to m sin i of around {{Jupiter mass|0.4}} and {{Jupiter mass|1}}, at distances of ~0.9 AU and ~4 AU, where i is the orbital inclination and m is the planet's actual mass. In 2023, the presence of a second, Jupiter-mass planet orbiting at 4 AU (75 Ceti c) was confirmed, which is more irradiated than Earth as well. The shorter period signal corresponding to a possible planet at 0.9 AU was found to be an alias of the true period of planet c.

{{OrbitboxPlanet begin

| table_ref =

| period_unit = day

}}

{{OrbitboxPlanet

| exoplanet = b

| semimajor = {{val|1.912|0.002|0.003}}

| eccentricity = {{val|0.093|0.026|0.042}}

| period = {{val|696.62|1.33|1.69}}

| mass = {{val|2.479|0.074|0.090|p=≥}}

}}

{{OrbitboxPlanet

| exoplanet = c

| semimajor = {{val|3.929|0.058|0.052}}

| eccentricity = {{val|0.023|0.191|0.003}}

| period = {{val|2051.62|45.98|40.47}}

| mass = {{val|0.912|0.088|0.143|p=≥}}

}}

References

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{{cite journal

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{{cite journal

| title=Substellar Companions to Seven Evolved Intermediate-Mass Stars

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| journal=Publications of the Astronomical Society of Japan

| volume=64 | issue=6 | at=135 | year=2012

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{{cite journal |last1=Mugrauer |first1=M. |date=December 2019 |title=Search for stellar companions of exoplanet host stars by exploring the second ESA-Gaia data release |journal=Monthly Notices of the Royal Astronomical Society |volume=490 |issue=4 |pages=5088–5102 |doi=10.1093/mnras/stz2673 |doi-access=free |bibcode=2019MNRAS.490.5088M}}

{{cite journal |last1=Teng |first1=Huan-Yu |last2=Sato |first2=Bun'ei |display-authors=etal |date=August 2023 |title=Revisiting planetary systems in the Okayama Planet Search Program: A new long-period planet, RV astrometry joint analysis, and a multiplicity-metallicity trend around evolved stars |journal=Publications of the Astronomical Society of Japan |volume=75 |issue=6 |pages=1030–1071 |doi=10.1093/pasj/psad056 |arxiv=2308.05343 |bibcode=2023PASJ...75.1030T}}

}}

Category:K-type giants

Category:Horizontal-branch stars

Category:Planetary systems with two confirmed planets

Category:Binary stars