Cannabaceae

Gliese 849
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Aquarius
Right ascension 22h 09m 40.34431s[1]
Declination –04° 38′ 26.6508″[1]
Apparent magnitude (V) 10.41[2]
Characteristics
Evolutionary stage Main sequence[3]
Spectral type M3.5V[4]
U−B color index 1.055[2]
B−V color index 1.531±0.035[2]
V−R color index 1.12[2]
R−I color index 1.41[2]
Astrometry
Radial velocity (Rv)−15.26±0.10[2] km/s
Proper motion (μ) RA: 1,132.583(39) mas/yr[1]
Dec.: −22.157(37) mas/yr[1]
Parallax (π)113.4447 ± 0.0300 mas[1]
Distance28.750 ± 0.008 ly
(8.815 ± 0.002 pc)
Absolute magnitude (MV)10.62[2]
Details[5]
Mass0.465±0.011 M
Radius0.464±0.018 R
Luminosity0.02887±0.00025 L
Surface gravity (log g)4.771±0.032 cgs
Temperature3,467±68[6] K
Metallicity [Fe/H]0.09±0.09[6] dex
Rotation40.45+0.19
−0.18
 d
[6]
Rotational velocity (v sin i)2.4[3] km/s
Other designations
BD−05°5715, GJ 849, HIP 109388, LFT 1689, LHS 517, LPM 814, LTT 8889, NLTT 53078, GCRV 13921, 2MASS J22094029-0438267[7]
Database references
SIMBADdata
Exoplanet Archivedata
ARICNSdata
Planet
Gliese 849b data Archived 2019-06-05 at the Wayback Machine

Gliese 849, or GJ 849, is a small, solitary star in the equatorial constellation of Aquarius. It has a reddish hue and is invisible to the naked eye with an apparent visual magnitude of 10.41.[2] The distance to this star is 28.8 light-years (8.8 parsecs) based on parallax,[1] but it is drifting closer to the Sun with a radial velocity of −15.3 km/s.[2] It has a pair of confirmed gas giant companions.[8]

The stellar classification of GJ 849 is M3.5V,[4] which means this is a small red dwarf star generating energy through hydrogen fusion at its core region. Various studies have found super-solar abundances in the spectra,[8] indicating that the elemental abundances of higher mass elements is significantly higher than in the Sun. The star has about half the mass and size of the Sun,[3] and is spinning slowly with a rotation period of approximately 39 days.[9] The estimated age of the star is more than three billion years.[3] It is radiating a mere 2.9%[5] of the luminosity of the Sun from its photosphere at an effective temperature of 3,490 K.[5]

Planetary system[edit]

In late 2006, a long-period Jupiter-like exoplanet was reported to be orbiting the red dwarf in a period just over 5 years in length. There was also a linear trend in the radial velocities which suggested another longer period companion.[3] The trend in the radial velocities was confirmed in 2013.[10] An orbit for the second exoplanet was finally determined in 2015. The first planet discovered, Gliese 849 b, was the first planet discovered orbiting a red dwarf with a semi-major axis greater than 0.21 AU.[8]

The Gliese 849 planetary system[6]
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
b ≥0.893+0.094
−0.097
 MJ
2.32+0.11
−0.13
1925.31±6.5 0.029±0.019
c ≥0.99±0.11 MJ 4.95+0.25
−0.28
5990+110
−100
0.092+0.038
−0.036

See also[edit]

References[edit]

  1. ^ a b c d e 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. ^ a b c d e f g h i Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  3. ^ a b c d e Butler, R. Paul; et al. (2006). "A Long-Period Jupiter-Mass Planet Orbiting the Nearby M Dwarf GJ 849". Publications of the Astronomical Society of the Pacific. 118 (850): 1685–1689. arXiv:astro-ph/0610179. Bibcode:2006PASP..118.1685B. doi:10.1086/510500. S2CID 14787596.
  4. ^ a b Schweitzer, A.; et al. (May 2019). "The CARMENES search for exoplanets around M dwarfs. Different roads to radii and masses of the target stars". Astronomy & Astrophysics. 625: 16. arXiv:1904.03231. Bibcode:2019A&A...625A..68S. doi:10.1051/0004-6361/201834965. S2CID 102351979. A68.
  5. ^ a b c Pineda, J. Sebastian; Youngblood, Allison; France, Kevin (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal. 918 (1): 23. arXiv:2106.07656. Bibcode:2021ApJ...918...40P. doi:10.3847/1538-4357/ac0aea. S2CID 235435757. 40.
  6. ^ a b c d Pinamonti, M.; Barbato, D.; et al. (June 2023). "The GAPS programme at TNG. XLVI. Deep search for low-mass planets in late-dwarf systems hosting cold Jupiters". Astronomy & Astrophysics. 677. arXiv:2306.04419. Bibcode:2023A&A...677A.122P. doi:10.1051/0004-6361/202346476. S2CID 259095781.
  7. ^ "BD-05 5715". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-02-20.
  8. ^ a b c Feng, Y. Katherina; et al. (2015). "The California Planet Survey IV: A Planet Orbiting the Giant Star HD 145934 and Updates to Seven Systems with Long-period Planets". The Astrophysical Journal. 800 (1). 22. arXiv:1501.00633. Bibcode:2015ApJ...800...22F. doi:10.1088/0004-637X/800/1/22. S2CID 56390823.
  9. ^ Suárez Mascareño, A.; et al. (September 2015), "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators", Monthly Notices of the Royal Astronomical Society, 452 (3): 2745–2756, arXiv:1506.08039, Bibcode:2015MNRAS.452.2745S, doi:10.1093/mnras/stv1441, S2CID 119181646.
  10. ^ Bonfils, Xavier; Delfosse, Xavier; Udry, Stéphane; Forveille, Thierry; Mayor, Michel; Perrier, Christian; Bouchy, François; Gillon, Michaël; Lovis, Christophe; Pepe, Francesco; Queloz, Didier; Santos, Nuno C.; Ségransan, Damien; Bertaux, Jean-Loup (2011). "The HARPS search for southern extra-solar planets XXXI. The M-dwarf sample". Astronomy and Astrophysics. 549: A109. arXiv:1111.5019. Bibcode:2013A&A...549A.109B. doi:10.1051/0004-6361/201014704. S2CID 119288366.

External links[edit]


One thought on “Cannabaceae

  1. Well, that’s interesting to know that Psilotum nudum are known as whisk ferns. Psilotum nudum is the commoner species of the two. While the P. flaccidum is a rare species and is found in the tropical islands. Both the species are usually epiphytic in habit and grow upon tree ferns. These species may also be terrestrial and grow in humus or in the crevices of the rocks.
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