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Revision as of 20:35, 16 January 2010 editMike s (talk | contribs)Extended confirmed users21,550 edits add reference section and references← Previous edit Revision as of 20:44, 16 January 2010 edit undoMike s (talk | contribs)Extended confirmed users21,550 edits update orbitbox numbers and add referenceNext edit →
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In 2003, the ] ] was discovered in the ] by ], ], ], and ].<ref>{{cite journal | url=http://www.iop.org/EJ/article/0004-637X/582/1/455/56131.html | author=Butler ''et al.'' | title=Seven New Keck Planets Orbiting G and K Dwarfs | journal=The ] | year=2003 | volume=582 | issue=1 | pages=455–466 | doi=10.1086/344570}}</ref> This planet receives the ] most similar to ] of any ]. In 2005, further observations revealed this star has another jovian planet orbiting further out, designated as ].<ref>{{cite journal | url=http://www.iop.org/EJ/article/0004-637X/632/1/638/62043.html | author=Vogt ''et al.'' | title=Five New Multicomponent Planetary Systems| journal=The ]| year=2005 | volume=632 | issue=1 | pages=638–658 | doi=10.1086/432901}}</ref> Those two planets are in a 4:1 orbital resonance. This means if HD 108874 b orbits the star four times, then HD 108874 c orbits only once, because the ] for planet c is four times longer than planet b. In 2003, the ] ] was discovered in the ] by ], ], ], and ].<ref>{{cite journal | url=http://www.iop.org/EJ/article/0004-637X/582/1/455/56131.html | author=Butler ''et al.'' | title=Seven New Keck Planets Orbiting G and K Dwarfs | journal=The ] | year=2003 | volume=582 | issue=1 | pages=455–466 | doi=10.1086/344570}}</ref> This planet receives the ] most similar to ] of any ]. In 2005, further observations revealed this star has another jovian planet orbiting further out, designated as ].<ref>{{cite journal | url=http://www.iop.org/EJ/article/0004-637X/632/1/638/62043.html | author=Vogt ''et al.'' | title=Five New Multicomponent Planetary Systems| journal=The ]| year=2005 | volume=632 | issue=1 | pages=638–658 | doi=10.1086/432901}}</ref> Those two planets are in a 4:1 orbital resonance. This means if HD 108874 b orbits the star four times, then HD 108874 c orbits only once, because the ] for planet c is four times longer than planet b.


{{OrbitboxPlanet begin}} {{OrbitboxPlanet begin
| table_ref = <ref name="Wright2009"> {{cite journal | url=http://www.iop.org/EJ/abstract/0004-637X/693/2/1084/ | author=Wright ''et al.'' | title=Ten New and Updated Multi-planet Systems, and a Survey of Exoplanetary Systems| journal=The ] | volume=693 | issue=2 | year=2009 | pages=1084–1099 | format=abstract | doi=10.1088/0004-637X/693/2/1084 }}()</ref>}}
{{OrbitboxPlanet {{OrbitboxPlanet
| exoplanet = ] | exoplanet = ]
| mass = >1.36 ± 0.13 | mass = >1.34 ± 0.11
| period = 395.4 ± 2.5 | period = 394.48 ± 0.60
| semimajor = 1.051 ± 0.02 | semimajor = 1.053 ± 0.061
| eccentricity = 0.07 ± 0.04 | eccentricity = 0.128 ± 0.022
}} }}
{{OrbitboxPlanet {{OrbitboxPlanet
| exoplanet = ] | exoplanet = ]
| mass = >1.018 ± 0.3 | mass = >1.064 ± 0.099
| period = 1605.8 ± 88 | period = 1680 ± 24
| semimajor = 2.68 ± 0.25 | semimajor = 2.77 ± 0.16
| eccentricity = 0.25 ± 0.07 | eccentricity = 0.273 ± 0.040
}} }}
{{Orbitbox end}} {{Orbitbox end}}

Revision as of 20:44, 16 January 2010

HD 108874

Orbits around the star HD108874
Observation data
Epoch J2000      Equinox J2000
Constellation Coma Berenices
Right ascension 12 30 26.8829
Declination +22° 52′ 47.383″
Apparent magnitude (V) 8.76
Characteristics
Spectral type G5 V
B−V color index 0.764
V−R color index 0.4
R−I color index 0.4
Variable type ”None”
Astrometry
Radial velocity (Rv)-30.7 km/s
Proper motion (μ) RA: -45.05 mas/yr
Dec.: -105.39 mas/yr
Parallax (π)14.59 ± 1.24 mas
Distance220 ± 20 ly
(69 ± 6 pc)
Absolute magnitude (MV)3.72
Details
Mass1 M☉
Radius1.22 R☉
Luminosity1.14 L☉
Temperature5407 K
Metallicity=+0.14
Rotation37.82 days
Age7.26 Giga- years
Other designations
BD+23°2466, HIP 61028, SAO 82344
Database references
SIMBADdata

HD 108874 is a yellow dwarf star (spectral type G5 V) in the constellation of Coma Berenices. It is 223 light years from Earth and has two extrasolar planets that are possibly in a 4:1 orbital resonance.

Star

HD 108874 is 2.7 billion years older than our Sun. The star has a temperature of 5407 K and luminosity 1.14 solar. It has metallicity 1.38 times solar, meaning this star has greater iron abundance relative to hydrogen and helium. It has mass about the same as the Sun, but the radius is 22% greater.

Planetary system

In 2003, the jovian planet HD 108874 b was discovered in the United States by Paul Butler, Geoffrey Marcy, Steven Vogt, and Debra Fischer. This planet receives the insolation most similar to Earth of any extrasolar planet. In 2005, further observations revealed this star has another jovian planet orbiting further out, designated as HD 108874 c. Those two planets are in a 4:1 orbital resonance. This means if HD 108874 b orbits the star four times, then HD 108874 c orbits only once, because the orbital period for planet c is four times longer than planet b.

The HD 108874 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b >1.34 ± 0.11 MJ 1.053 ± 0.061 394.48 ± 0.60 0.128 ± 0.022 — —
c >1.064 ± 0.099 MJ 2.77 ± 0.16 1680 ± 24 0.273 ± 0.040 — —

See also

References

  1. Butler; et al. (2003). "Seven New Keck Planets Orbiting G and K Dwarfs". The Astrophysical Journal. 582 (1): 455–466. doi:10.1086/344570. {{cite journal}}: Explicit use of et al. in: |author= (help)
  2. Vogt; et al. (2005). "Five New Multicomponent Planetary Systems". The Astrophysical Journal. 632 (1): 638–658. doi:10.1086/432901. {{cite journal}}: Explicit use of et al. in: |author= (help)
  3. Wright; et al. (2009). "Ten New and Updated Multi-planet Systems, and a Survey of Exoplanetary Systems" (abstract). The Astrophysical Journal. 693 (2): 1084–1099. doi:10.1088/0004-637X/693/2/1084. {{cite journal}}: Explicit use of et al. in: |author= (help)(web Preprint)

External links

Categories: