Gamma Delphini, which isLatinized from γ Delphini, is a widebinary star system in the northernconstellation ofDelphinus. The star marks one corner of theasterism "Job's Coffin". The pair can be split with a modestamateur telescope and have been described as "one of the prettier pairs in the sky", with their contrasting colors said to be orange and lime in appearance.[11] Together, the system is visible to the naked eye with a combinedapparent visual magnitude of 3.87.[12]
This star was found to be adouble by Christian Mayer and later observed by William Herschel on Sept 27th, 1779.[citation needed] It was later included as STF 2727 in the catalogue compiled by F. G. W. Struveand can be found under this name in the Washington Double Star Catalog. At the time, the components had anangular separation of12.0″ along aposition angle (PA) of 280°. As of 2019, they are separated by8.90″ with a PA of 265°. The fainter component, designated γ1 Delphini, is ofapparent magnitude 5.03. Its companion is a magnitude 4.360 star designated γ2 Delphini.[3] A fit oforbital elements to the available positional data provides aperiod of 3,249 years with a higheccentricity (ovalness) of 0.88.[9] Their physical separation ranges from roughly 40 out to600 AU.[12]
The brighter component, γ2 Delphini, has an orange hue with a class of K1IV.[6] Being the more massive star of the pair, it is the moreevolved star and is currently on thesubgiant branch.[5] It has double the mass of the Sun but has expanded to over eight times the Sun's radius. The star is radiating 33 times the luminosity of the Sun at 4,798 K.[7] It is spinning with aprojected rotational velocity of 3.6 km/s.[10] The star displays a radial acceleration with a periodicity of 1.44 years, which may be the effect of an orbiting companion.[15]
In 1999, the presence of a planetary companion was inferred around Gamma2 Delphini as one possible explanation for the radial velocity variations.[15] Such a planet would have a minimum mass of 0.7Jupiter masses, orbital period of 1.44 years and separation of nearly 1.5astronomical units (almost the orbital separation ofMars from theSun). The planetary candidate has not been confirmed. McDonald Observatory researches have set mass limits for potential planetary companions in orbit around the star Gamma2 Delphini.[17]
^abMassarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity",The Astronomical Journal,135 (1):209–231,Bibcode:2008AJ....135..209M,doi:10.1088/0004-6256/135/1/209
^abIrwin, A. W.; et al. (1999), Hearnshaw, J. B.; Scarfe, C. D. (eds.), "A Program for the Analysis of Long-Period Binaries: The Case of γ Delphini",Precise Stellar Radial Velocities. IAU Colloquium 170, ASP Conference Series #185, vol. 185, p. 297,Bibcode:1999ASPC..185..297I,ISBN1-58381-011-0{{citation}}: CS1 maint: work parameter with ISBN (link)
^Haakonsen, Christian Bernt; Rutledge, Robert E. (September 2009), "XID II: Statistical Cross-Association of ROSAT Bright Source Catalog X-ray Sources with 2MASS Point Source Catalog Near-Infrared Sources",The Astrophysical Journal Supplement,184 (1):138–151,arXiv:0910.3229,Bibcode:2009ApJS..184..138H,doi:10.1088/0067-0049/184/1/138,S2CID119267456.
