HD 125595

HD 125595 is a 9th magnitude K-type main sequence star located approximately 89 light years away in the constellation Centaurus. This star is smaller, cooler, dimmer, and less massive than our Sun. Also its metal content is 4% more than the Sun. In 2009, a gas giant planet was found in orbit around the star.

HD 125595
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Centaurus
Right ascension  14h 21m 23.186s[1]
Declination −40° 23′ 38.21″[1]
Apparent magnitude (V) 9.03
Characteristics
Spectral type K4V[2]
Apparent magnitude (B) 10.13
Apparent magnitude (J) 7.097
Apparent magnitude (H) 6.608
Apparent magnitude (K) 6.447
B−V color index 1.10
Astrometry
Radial velocity (Rv)3.1 km/s
Proper motion (μ) RA: −561.46 ± 1.05[1] mas/yr
Dec.: −67.06 ± 0.85[1] mas/yr
Parallax (π)35.77 ± 1.04[1] mas
Distance91 ± 3 ly
(28.0 ± 0.8 pc)
Absolute magnitude (MV)6.84
Details
Mass0.68 M☉
Radius0.78 ± 0.07 R☉
Luminosity0.239 ± 0.020 L☉
Surface gravity (log g)4.29 cgs
Temperature4590 ± 100 K
Metallicity0.02
Rotation37.2±2.0 d[2]
Other designations
CD−39°8857, GCRV 64739, Gliese 545.1, HIP 70170, LHS 2900, LPM 523, LTT 5648, NLTT 37029, PPM 319432
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

Planetary system

HD 125595 b is an extrasolar planet which orbits the star. This planet has at least 14 times the mass of Earth and takes 9 days and 16 hours to orbit the star at a semimajor axis of 0.081 AU.[3]

The HD 125595 planetary system[3]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥0.045 MJ 0.0809 ± 0.0014 9.6737 ± 0.0039 0 — —
gollark: Yeeees.
gollark: Can you rephrase that? Your unclearness is unclear.
gollark: Tor hidden services are magically routed over the Tor network via magic; you don't go through Tor to an exit node to a hidden service.
gollark: No, that's not how they work.
gollark: LyricLy, you WILL call with current continuation.

See also
  • List of extrasolar planets

References
  1. 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
  2. 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.
  3. Ségransan, D.; et al. (2011). "The HARPS search for southern extra-solar planets. XXIX. Four new planets in orbit around the moderately active dwarfs HD 63765, HD 104067, HD 125595, and HIP 70849". Astronomy and Astrophysics. 535. A54. arXiv:1107.0339. Bibcode:2011A&A...535A..54S. doi:10.1051/0004-6361/200913580.


This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.