HD 154345 b

Last updated
HD 154345 b
HD154345B.jpg
Planet HD 154345 b (min mass ~1 MJ) in the background with two hypothetical moons visible. Image was created with Celestia V1.41 using a custom map for the Planet and its moons
Discovery [1]
Discovered by Wright et al.
Discovery site United States
Discovery dateMarch 12, 2006
(published: May 27, 2007)
radial velocity
Orbital characteristics [2]
4.2+0.14
−0.15  AU
Eccentricity 0.157+0.03
−0.029
3342±40  d
9.15±0.11  yr
Average orbital speed
13.7
Inclination 69°+13°
−12° or 111°+12°
−13°
77°+38°
−53°
2458428+72
−116
319.6°+8.7°
−8.4°
Semi-amplitude 14.28 ± 0.75
Star HD 154345
Physical characteristics [2]
Mass 1.19+0.14
−0.11  MJ

    HD 154345 b is a Jupiter-mass extrasolar planet orbiting the star HD 154345.

    Contents

    Discovery

    Wright et al. discovered the planet in March 2006 using the radial velocity method to detect the small wobbling movement of the star caused by the gravity of the planet. The discovery was published in May 2007. [1]

    While the existence of HD 154345 b has been unclear due to the correlation of its orbital period with the star's activity cycle, [3] a study in 2021 further confirmed its planetary nature. [4] In 2023, the inclination and true mass of HD 154345 b were determined via astrometry. [2]

    Characteristics

    The planet has a mass slightly greater than that of Jupiter. It orbits its parent star at a distance of 4.18 AU. Its orbital period is about 9.15 Earth years and its orbit is near-circular. [2] There are no interior planets of minimum mass (m sini) greater than 0.3 Jupiter. [5] Jupiter-like planets with these orbital and system characteristics are unlikely to be perturbed from the star's inclination. [6] Since the star's inclination is known as around 50°, this would make the planet's most likely mass greater than Jupiter's mass but less than twice that mass. [7]

    As such HD 154345 b is presumed to be a gas giant "Jupiter twin". [5] Depending on composition the two planets may be around the same size, or HD 154345 b may be larger. This planet may also harbor a system of moons and rings.[ citation needed ]

    See also

    Related Research Articles

    HD 169830 is a star in the southern constellation of Sagittarius. It has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.90. The star is located at a distance of 120 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −17.3 km/s, and is predicted to come as close as 20.7 ly (6.4 pc) in 2.08 million years. HD 169830 is known to be orbited by two large Jupiter-like exoplanets.

    <span class="mw-page-title-main">54 Piscium</span> Orange dwarf star in the constellation Pisces

    54 Piscium is an orange dwarf star approximately 36 light-years away in the constellation of Pisces. In 2003, an extrasolar planet was confirmed to be orbiting the star, and in 2006, a brown dwarf was also discovered orbiting it.

    <span class="mw-page-title-main">Tau Boötis b</span> Hot Jupiter orbiting Tau Boötis A

    Tau Boötis b, or more precisely Tau Boötis Ab, is an extrasolar planet approximately 51 light-years away. The planet and its host star is one of the planetary systems selected by the International Astronomical Union as part of NameExoWorlds, their public process for giving proper names to exoplanets and their host star. The process involved public nomination and voting for the new names, and the IAU planned to announce the new names in mid-December 2015. However, the IAU annulled the vote as the winning name was judged not to conform with the IAU rules for naming exoplanets.

    HD 38529 is a binary star approximately 138 light-years away in the constellation of Orion.

    HD 1237 is a binary star system approximately 57 light-years away in the constellation of Hydrus.

    <span class="mw-page-title-main">HD 28185 b</span> Gas giant orbiting HD 28185

    HD 28185 b is an extrasolar planet 128 light-years away from Earth in the constellation of Eridanus. The planet was discovered orbiting the Sun-like star HD 28185 in April 2001 as a part of the CORALIE survey for southern extrasolar planets, and its existence was independently confirmed by the Magellan Planet Search Survey in 2008. HD 28185 b orbits its sun in a circular orbit that is at the inner edge of its star's habitable zone.

    HD 102195 is an orange-hued star in the zodiac constellation of Virgo with a confirmed exoplanet companion. With an apparent visual magnitude of 8.07, the star is too faint to be seen with the naked eye. The distance to HD 102195 can be estimated from its annual parallax shift of 34.06 mas, yielding a separation of 95.8 light years. It is moving further away from the Earth with a heliocentric radial velocity of 1.85 km/s. This is a high proper motion star and a possible member of the η Cha stellar kinematic group.

    <span class="mw-page-title-main">Gliese 876 c</span> Gas giant orbiting Gliese 876

    Gliese 876 c is an exoplanet orbiting the red dwarf Gliese 876, taking about 30 days to complete an orbit. The planet was discovered in April 2001 and is the second planet in order of increasing distance from its star.

    <span class="mw-page-title-main">Doppler spectroscopy</span> Indirect method for finding extrasolar planets and brown dwarfs

    Doppler spectroscopy is an indirect method for finding extrasolar planets and brown dwarfs from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star.

    HD 164922 b is an exoplanet orbiting the star HD 164922 about 72 light-years from Earth in the constellation Hercules. Its inclination is not known, and its true mass may be significantly greater than the radial velocity lower limit of 0.36 Jupiter masses. The planet also has a low eccentricity, unlike most other long period extrasolar planets – 0.05 – about the same as Jupiter and Saturn in the Solar System. The exoplanet was found by using the radial velocity method, from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star.

    HD 66428 is a G-type main sequence star located approximately 174 light-years away in the constellation of Monoceros. This star is similar to the Sun with an apparent magnitude of 8.25, an effective temperature of 5705 ± 27 K and a solar luminosity 1.28. Its absolute magnitude is 11.1 while its U-V color index is 0.71. It is considered an inactive star and it is metal-rich . This star has a precise mass of 1.14552 solar masses. This precision comes from the Corot mission that measured asteroseismology.

    HD 154345 is a star in the northern constellation of Hercules. With an apparent visual magnitude of +6.76 it is a challenge to view with the naked eye, but using binoculars it is an easy target. The distance to this star is 59.6 light years based on parallax, but it is drifting closer with a radial velocity of −47 km/s. At least one exoplanet is orbiting this star.

    Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.

    HD 92788 is a star in the equatorial constellation of Sextans. It has a yellow hue but is too dim to be visible to the naked eye, having an apparent visual magnitude of 7.31. The star is located at a distance of 113 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −4.5 km/s. Two planets have been found in orbit around the star.

    HD 24040 is a metal-rich G-type star located approximately 152 light-years away in the constellation of Taurus. In 2006 a long-period planet was discovered.

    HIP 14810 c is an extrasolar planet approximately 165 light-years away in the constellation of Aries. This planet has mass at least 1.28 times that of Jupiter and orbits at 0.545 AU in an eccentric orbit. The planet was discovered by the N2K Consortium in 2006 and announced in a paper published in 2007. With the discovery of a third planet in the system which was announced in 2009, the parameters of this planet were revised.

    HD 210277 b is an extrasolar planet orbiting the star HD 210277. It was discovered in September 1998 by the California and Carnegie Planet Search team using the highly successful radial velocity method. The planet is at least 24% more massive than Jupiter. The mean distance of the planet from the star is slightly more than Earth's distance from the Sun. However, the orbit is very eccentric, so at periastron this distance is almost halved, and at apastron it is as distant as Mars is from the Sun.

    HD 30177 b is an extrasolar planet located approximately 181.6 light-years away in the constellation of Dorado, orbiting the star HD 30177.

    <span class="mw-page-title-main">Upsilon Andromedae e</span> Extrasolar planet in the Andromeda constellation

    Upsilon Andromedae e is the proposed outermost extrasolar planet orbiting the star Upsilon Andromedae in the constellation of Andromeda. If it exists, this planet would be one of the most Jupiter-like exoplanets found in terms of mass and semi-major axis. However, subsequent studies have found that the apparent planetary signal is more likely to be an instrumental artifact.

    HD 30562 b is an extrasolar planet which orbits the F-type main sequence star HD 30562, located approximately 85.4 light years away in the constellation Eridanus.

    References

    1. 1 2 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. S2CID   35682784.
    2. 1 2 3 4 Xiao, Guang-Yao; Liu, Yu-Juan; et al. (March 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements". Research in Astronomy and Astrophysics . arXiv: 2303.12409 .
    3. ↑ Wright, J. T. (October 2015). Boisse, I.; Demangeon, O.; Bouchy, F.; Arnold, L. (eds.). Twenty Years of Precise Radial Velocities at Keck and Lick Observatories. Proceedings of colloquium 'Twenty years of giant exoplanets' held at Observatoire de Haute Provence, France, October 5-9, 2015. Observatoire de Haute-Provence, Institut Pythéas. pp. 8–17. arXiv: 1603.08384 . Bibcode:2015tyge.conf....8W.
    4. ↑ Rosenthal, Lee J.; Fulton, Benjamin J.; Hirsch, Lea A.; Isaacson, Howard T.; Howard, Andrew W.; Dedrick, Cayla M.; Sherstyuk, Ilya A.; Blunt, Sarah C.; Petigura, Erik A.; Knutson, Heather A.; Behmard, Aida; Chontos, Ashley; Crepp, Justin R.; Crossfield, Ian J. M.; Dalba, Paul A.; Fischer, Debra A.; Henry, Gregory W.; Kane, Stephen R.; Kosiarek, Molly; Marcy, Geoffrey W.; Rubenzahl, Ryan A.; Weiss, Lauren M.; Wright, Jason T. (2021). "The California Legacy Survey. I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades". The Astrophysical Journal Supplement Series. 255 (1): 8. arXiv: 2105.11583 . Bibcode:2021ApJS..255....8R. doi:10.3847/1538-4365/abe23c. S2CID   235186973.
    5. 1 2 Wright, J. T.; et al. (2008). "The Jupiter Twin HD 154345b". The Astrophysical Journal Letters. 683 (1): L63–L66. arXiv: 0802.1731 . Bibcode:2008ApJ...683L..63W. doi:10.1086/587461. S2CID   16808434.
    6. ↑ Roberto Sanchis-Ojeda; Josh N. Winn; Daniel C. Fabrycky (2012). "Starspots and spin-orbit alignment for Kepler cool host stars". Astronomische Nachrichten. 334 (1–2): 180–183. arXiv: 1211.2002 . Bibcode:2013AN....334..180S. doi:10.1002/asna.201211765. S2CID   38743202.
    7. ↑ Simpson, E. K.; et al. (November 2010), "Rotation periods of exoplanet host stars", Monthly Notices of the Royal Astronomical Society , 408 (3): 1666–1679, arXiv: 1006.4121 , Bibcode:2010MNRAS.408.1666S, doi:10.1111/j.1365-2966.2010.17230.x, S2CID   6708869

    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.