Planet-hosting star
Most stars are accompanied by planets, though the exact proportion remains uncertain due to current limitations in detecting distant exoplanets.Thus many known exoplanets are "Hot Jupiters", planets of Jovian mass or larger in very small orbits with periods of only a few days.In addition, statistical analyses indicate that lower-mass stars (red dwarfs, of spectral category M) are less likely to have planets massive enough to be detected by the radial-velocity method.[12] However, this type of massive star eventually evolves into a cooler red giant that rotates more slowly and thus can be measured using the radial-velocity method.Observations using the Spitzer Space Telescope indicate that extremely massive stars of spectral category O, which are much hotter than the Sun, produce a photo-evaporation effect that inhibits planetary formation.[14] Fallback disks of matter that failed to escape orbit during a supernova may form planets around neutron stars and black holes.[21] However, this claimed relationship has become a point of contention in the planetary astrophysics community, being frequently denied[22][23] but also supported.[26] More than one hundred planets have been discovered orbiting one member of a binary star system (e.g. 55 Cancri, possibly Alpha Centauri Bb),[27] and several circumbinary planets have been discovered which orbit around both members of a binary star (e.g. PSR B1620-26 b, Kepler-16b).Another surprising Kepler finding is circumbinary planets tend to orbit their stars close to the critical instability radius (theoretical calculations indicate the minimum stable separation is roughly two to three times the size of the stars' separation).
planetsplanetary systemsSun-like starshabitable zoneradial-velocityHot JupitersJovianspectral classesmetallicitygravitational microlensingMilky Waymain-sequence starsspectral categoriesred dwarfsspectral categoryradial-velocity methodKepler space telescopetransit methodred giantSpitzer Space Telescopephoto-evaporationsupernovanatal kickneutron starsblack holesmicrolensingNeptunebrown dwarfssub-brown dwarfsOTS 44Rogue planetshydrogenheliummetalslogarithmic scalegas giantsprotoplanetary disksplanetary coresmigratedlithiumbinary star55 CancriAlpha Centauri Bbcircumbinary planetsPSR B1620-26 bKepler-16btriple star16 Cygni BbKepler 6430 ArietisKeplereclipsing binariesspeckle imagingradial velocityKepler-132Kepler-296open clustersopen clusterNGC 6811Kepler-66Kepler-67G-type starK-type starsNatureBibcodeProgress of Theoretical Physics SupplementGeoffrey W. MarcyProceedings of the National Academy of SciencesSpitzer Science CenterWayback MachineRosalba PernaSky & TelescopeIlaria PascucciFormationAccretionMolecular cloudBok globuleYoung stellar objectProtostarPre-main-sequenceHerbig Ae/BeT TauriHerbig–Haro objectHayashi trackHenyey trackEvolutionMain sequenceRed-giant branchHorizontal branchRed clumpAsymptotic giant branchpost-AGBsuper-AGBBlue loopPlanetary nebulaProtoplanetaryWolf–Rayet nebulaPG1159Dredge-upInstability stripLuminous blue variableStellar populationSuperluminousHypernovaClassificationSubdwarfSubgiantYellowBright giantSupergiantHypergiantCarbonWhite dwarfChemically peculiarHe-weakBariumLambda BoötisTechnetiumExtremeBlue stragglerRemnantsCompact starParker's starHelium planetNeutronRadio-quiet