47 Ursae Majoris

47 Ursae Majoris (abbreviated 47 UMa), formally named Chalawan /ˈtʃɑːləwən/,[7][8] is a yellow dwarf star approximately 45.3 light-years[1] from Earth in the constellation of Ursa Major. As of 2011, three extrasolar planets (designated 47 Ursae Majoris b, c and d; the first two later named Taphao Thong and Taphao Kaew) are believed to orbit the star.

47 Ursae Majoris / Chalawan

Location of 47 Ursae Majoris in Ursa Major
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ursa Major
Right ascension 10h 59m 27.9728s[1]
Declination +40° 25′ 48.921″[1]
Apparent magnitude (V) +5.03
Characteristics
Spectral type G1V
U−B color index 0.13
B−V color index 0.61
Astrometry
Radial velocity (Rv)11.24(12)[1] km/s
Proper motion (μ) RA: −316.850(97) mas/yr[1]
Dec.: 55.180(118) mas/yr[1]
Parallax (π)72.0070 ± 0.0974 mas[1]
Distance45.30 ± 0.06 ly
(13.89 ± 0.02 pc)
Absolute magnitude (MV)4.41[2]
Details
Mass1.08[3] M☉
Radius1.172 ± 0.111[4] R☉
Luminosity1.48[note 1] L☉
Surface gravity (log g)4.377[3] cgs
Temperature5,887 ± 3.8[5] K
Metallicity110% solar[3]
Rotational velocity (v sin i)2.80[3] km/s
Age6.03[6] Gyr
Other designations
Chalawan, BD+41°2147, FK5 1282, GC 15087, GCTP 2556.00, Gliese 407, HD 95128, HIP 53721, HR 4277, LTT 12934, SAO 43557
Database references
SIMBADThe star
planet b
planet c
planet d
Exoplanet Archivedata
ARICNSdata
Extrasolar Planets
Encyclopaedia		data

The star is located fairly close to the Solar System: according to astrometric measurements made by the Gaia space observatory, it exhibits a parallax of 72.0070 milliarcseconds, corresponding to a distance of 45.30 light-years.[1] With an apparent magnitude of +5.03, it is visible to the naked eye and its absolute magnitude of +4.29 implies a visual luminosity around 60% greater than the Sun. A solar analog, with a spectral type of G1V, it has a similar mass to that of the Sun but is slightly hotter at around 5,882 K.[3] and slightly more metal-rich with around 110% of the solar abundance of iron.

Like the Sun, 47 Ursae Majoris is on the main sequence, converting hydrogen to helium in its core by nuclear fusion. Based on its chromospheric activity, the star may be around six billion years old, though evolutionary models suggest an older age of around 8.7 billion years.[6] Other studies have yielded estimates of 4.4 and 7 billion years for the star.[9] The low level of magnetic activity makes it a Maunder Minimum candidate star.[10]

Nomenclature

47 Ursae Majoris is the Flamsteed designation. On their discoveries the planets were successively designated 47 Ursae Majoris b, c and d.

In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars.[11] The process involved public nomination and voting for the new names.[12] In December 2015, the IAU announced the winning names were Chalawan for this star and Taphao Thong and Taphao Kaew for two of the planets (b and c, respectively).[13] The winning names were submitted by the Thai Astronomical Society, Thailand. Chalawan (Thai: ชาละวัน [t͡ɕʰāːlāwān]) is a mythological crocodile king from the Thai folktale Krai Thong and Taphaothong and Taphaokaeo are two sisters associated with the tale.[14] ('Chalawan' is also the name given to an extinct genus of crocodylian. It contains a single species, Chalawan thailandicus.[15])

In 2016, the IAU organized a Working Group on Star Names (WGSN)[16] to catalog and standardize proper names for stars. In its first bulletin of July 2016,[17] the WGSN explicitly recognized the names of exoplanets and their host stars approved by the Executive Committee Working Group Public Naming of Planets and Planetary Satellites, including the names of stars adopted during the 2015 NameExoWorlds campaign. This star is now so entered in the IAU Catalog of Star Names.[7]

Planetary system

In 1996 an exoplanet (47 UMa b) was announced in orbit around 47 Ursae Majoris by Geoffrey Marcy and R. Paul Butler. The discovery was made by observing the Doppler shift of the star's spectrum corresponding to changes in the star's radial velocity as the planet's gravity pulled it around.[18] The planet was the first long-period extrasolar planet discovered. Unlike the majority of known such planets, it has a low-eccentricity orbit. The planet is at least 2.53 times the mass of Jupiter and takes 1,078 days, or 2.95 years, to orbit its star. If it were to be located in the Solar System, it would lie between the orbits of Mars and Jupiter.[19]

Orbits of the planets in the 47 Ursae Majoris system. The orbit of 47 UMa d is currently quite uncertain; both it and that of 47 UMa c may be circular.

In 2001, preliminary astrometric measurements made by the Hipparcos probe suggested the orbit of 47 UMa b is inclined at an angle of 63.1° to the plane of the sky, implying the planet's true mass is around 2.9 times that of Jupiter.[20] However, subsequent analysis suggested the Hipparcos measurements were not precise enough to accurately determine the orbits of substellar companions, and the inclination and true mass remain unknown.[21]

A second planet (47 UMa c) was announced in 2002 by Debra Fischer, Geoffrey Marcy and R. Paul Butler. The discovery was made using the same radial velocity method. According to Fischer et al., the planet takes around 2,391 days, or 6.55 years, to complete an orbit. This configuration is similar to the configuration of Jupiter and Saturn in the Solar System, with the orbital ratio (close to 5:2) and mass ratio roughly similar.[22] Subsequent measurements failed to confirm the existence of the second planet, and it was noted that the dataset used to determine its existence left the planet's parameters "almost unconstrained".[23] Analysis of a longer dataset spanning over 6,900 days suggests that while a second planet in the system is likely, periods near 2,500 days have a high false-alarm probability, and the best fit model gives an orbital period of 7,586 days at a distance of 7.73 AU from the star. Nevertheless, the parameters of the second planet are still highly uncertain.[24] On the other hand, the Catalog of Nearby Exoplanets gives a period of 2,190 days, which would put the planets close to a 2:1 ratio of orbital periods, though the reference for these parameters is uncertain: the original Fischer et al. paper is cited as a reference in spite of the fact that it gives different parameters,[22][25] though this solution has been adopted by the Extrasolar Planets Encyclopaedia.[26]

In 2010, the discovery of a third planet (47 UMa d) was made by using the Bayesian Kepler Periodogram. Using this model of this planetary system it was determined that it is 100,000 times more likely to have three planets than two planets. This discovery was announced by Debra Fischer and P. C. Gregory. This 1.64 MJ planet has an orbital period of 14,002 days, or 38.33 years, and a semi-major axis of 11.6 AU with a moderate eccentricity of 0.16.[19] It would be the longest-period planet discovered by the radial velocity method, although longer-period planets had previously been discovered by direct imaging and pulsar timing.

Simulations suggest that the inner part of the habitable zone of 47 Ursae Majoris could host a terrestrial planet in a stable orbit, though the outer regions of the habitable zone would be disrupted by the gravitational influence of the planet 47 UMa b.[27] However, the presence of a giant planet within 2.5 AU of the star may have disrupted planet formation in the inner system, and reduced the amount of water delivered to inner planets during accretion.[28] This may mean any terrestrial planets orbiting in the habitable zone of 47 Ursae Majoris are likely to be small and dry. As of 2008, there have been two METI messages sent to 47 Ursae Majoris. Both were transmitted from Eurasia's largest radar—70-metre (230 ft) Eupatoria Planetary Radar. The first message, the Teen Age Message, was sent on September 3, 2001, and it will arrive at 47 Ursae Majoris in July 2047. The second message, Cosmic Call 2, was sent on July 6, 2003, and it will arrive at 47 Ursae Majoris in May 2049.[29]

The 47 Ursae Majoris planetary system[19]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b (Taphao Thong) >2.53+0.07
−0.06 MJ		 2.10 ± 0.02 1,078 ± 2 0.032 ± 0.014 — —
c (Taphao Kaew) >0.540+0.066
−0.073 MJ		 3.6 ± 0.1 2,391+100
−70		 0.098+0.047
−0.096		 — —
d >1.64+0.29
−0.48 MJ		 11.6+2.1
−2.9		 14,002+4,018
−5,095		 0.16+0.09
−0.16		 — —

Because of its planetary system, 47 Ursae Majoris was listed as one of the top 100 target stars for NASA's former Terrestrial Planet Finder mission.[30]

See also

Notes
  1. From , where is the luminosity, is the radius, is the effective surface temperature and is the Stefan–Boltzmann constant.

References
  1. 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.
  2. Elgarøy, Øystein; Engvold, Oddbjørn; et al. (March 1999), "The Wilson-Bappu effect of the MgII K line - dependence on stellar temperature, activity and metallicity", Astronomy and Astrophysics, 343: 222–228, Bibcode:1999A&A...343..222E
  3. "Stars Table". Catalog of Nearby Exoplanets. Archived from the original on 17 October 2008. Retrieved 2008-10-04.
  4. G. T. van Belle; K. von Braun (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". Astrophysical Journal. 694 (2): 1085–1098. arXiv:0901.1206. Bibcode:2009ApJ...694.1085V. doi:10.1088/0004-637X/694/2/1085. S2CID 18370219.
  5. V. V. Kovtyukh; Soubiran, C.; et al. (2003). "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios". Astronomy and Astrophysics. 411 (3): 559–564. arXiv:astro-ph/0308429. Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378. S2CID 18478960.
  6. C. Saffe; Gómez, M.; et al. (2005). "On the Ages of Exoplanet Host Stars". Astronomy and Astrophysics. 443 (2): 609–626. arXiv:astro-ph/0510092. Bibcode:2005A&A...443..609S. doi:10.1051/0004-6361:20053452. S2CID 11616693.
  7. "IAU Catalog of Star Names". Retrieved 28 July 2016.
  8. Thai Astronomical Society, Chalawan, Taphao Thong, Taphao Kaew – First Thai Exoworld Names
  9. E. E. Mamajek; L. A. Hillenbrand (2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". Astrophysical Journal. 687 (2): 1264–1293. arXiv:0807.1686. Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. S2CID 27151456.
  10. Lubin, Dan; et al. (March 2012). "Frequency of Maunder Minimum Events in Solar-type Stars Inferred from Activity and Metallicity Observations". The Astrophysical Journal Letters. 747 (2): L32. Bibcode:2012ApJ...747L..32L. doi:10.1088/2041-8205/747/2/L32.
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  14. "NameExoWorlds The Approved Names". Archived from the original on 2018-02-01. Retrieved 2015-12-19.
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  17. "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
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  19. P. C. Gregory; D. A. Fischer (2010). "A Bayesian periodogram finds evidence for three planets in 47 Ursae Majoris". Monthly Notices of the Royal Astronomical Society. 403 (2): 731–747. arXiv:1003.5549. Bibcode:2010MNRAS.403..731G. doi:10.1111/j.1365-2966.2009.16233.x. S2CID 16722873.
  20. I. Han; D. C. Black; et al. (2001). "Preliminary Astrometric Masses for Proposed Extrasolar Planetary Companions". Astrophysical Journal Letters. 548 (1): L57–L60. Bibcode:2001ApJ...548L..57H. doi:10.1086/318927.
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  23. Naef, Dominique; Mayor, Michel; Beuzit, Jean-Luc; Perrier, Christian; Queloz, Didier; Sivan, Jean-Pierre; Udry, Stéphane (2004). "The ELODIE survey for northern extra-solar planets. III. Three planetary candidates detected with ELODIE" (PDF). Astronomy and Astrophysics. 414 (1): 351–359. arXiv:astro-ph/0310261. Bibcode:2004A&A...414..351N. doi:10.1051/0004-6361:20034091. S2CID 16603563.
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  28. S. Raymond (2006). "The Search for other Earths: limits on the giant planet orbits that allow habitable terrestrial planets to form". Astrophysical Journal Letters. 643 (2): L131–134. arXiv:astro-ph/0605136. Bibcode:2006ApJ...643L.131R. doi:10.1086/505596. S2CID 14298813.
  29. А. Л. Зайцев (7 June 2004). Передача и поиски разумных сигналов во Вселенной (PDF). Пленарный доклад на Всероссийской астрономической конференции ВАК-2004 "Горизонты Вселенной", Москва, МГУ (in Russian). Archived from the original on 30 May 2019. Retrieved 5 February 2008.
  30. "#72 HIP 53721". TPF-C Top 100. Retrieved 22 July 2006.
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