HD 106906 b is a directly imaged planetary-mass companion and candidate exoplanet orbiting the star, in the constellation Crux at about from Earth. It is estimated to be about eleven times the mass of Jupiter and is located about 738 AU away from its host star. is rare in science; while its mass estimate is nominally consistent with identifying it as an exoplanet, it appears at a much wider separation from its parent star than thought possible for in-situ formation from a protoplanetary disk.
Description
is the only known companion orbiting, a spectroscopic binary starcomposed of two F5Vmain-sequence stars with a combined mass of. Based on the star's luminosity and temperature, the system is estimated to be about. The system is a likely member of the Scorpius–Centaurus Association. The star is surrounded by a debris disk oriented 21 degrees away from ; this disk is about from the binary on its interior and ranges asymmetrically from approximately from the binary at its outer edge. Based on its near-infrared spectral-energy distribution, its age, and relevant evolutionary models, is estimated to be, with a surface temperature of. The high surface temperature, a relic of its recent formation, gives it a luminosity of about 0.02% of the Sun's. While its mass and temperature are similar to other planetary-mass companions/exoplanets like or, its projected separation from the star is much larger, about, giving it one of the widest orbits of any currently known planetary-mass companions. The measurements obtained thus far are not adequate to evaluate its orbital properties. If its eccentricity is large enough, it might approach the outer edge of the primary's debris disk closely enough to interact with it at periastron. In such a case, the outer extent of the debris disk would be truncated at the inner edge of Hill sphere at periastron. The discovery team evaluated the possibility that is not gravitationally bound to, but is seen close to it along our line of sight and moving in the same direction by chance. The odds of such a coincidence were found to be less than 0.01%.
Discovery
Observation of star began in 2005, utilizing the Magellan Telescopes at the Las Campanas Observatory in the Atacama Desert of Chile, some eight years before the companion was discovered. The initial interest in was directed largely to the debris disk surrounding the star, a pre-main-sequence member of Lower Centaurus Crux. On December 4, 2013, University of Arizona graduate student Vanessa Bailey, leader of an international team of astronomers, detailed the discovery of with a paper first published as a preprint on the arXiv and later as a refereed article in The Astrophysical Journal Letters.
Possible formation mechanism
The discovery team and astronomers worldwide were puzzled by extreme separation from its host star, because it is not considered possible that a star's protoplanetary disk could be extensive enough to permit formation of gas giants at such a distance. To account for the separation, it is theorized that the companion formed independently from its star as part of a binary system. This proposal is somewhat problematic in that the mass ratio of ~140:1 is not in the range expected from this process; binary stars typically do not exceed a ratio of 10:1. This is still considered preferable, however, to the alternate theory that the companion formed closer to its primary and then was scattered to its present distance by gravitational interaction with another orbital object. This second companion would need to have a mass greater than that of, and the discovery team found no such object beyond 35 AU from the primary. Additionally, the scattering process would have likely disrupted the protoplanetary disk. Subsequently, astronomer Paul Kalas and colleagues discovered that Hubble Space Telescope images show a highly asymmetric shape to the debris disk beyond a radius of 200 AU, supporting the hypothesis of a dynamical upheaval that involved the planet and another perturber, such as a second planet in the system or a close encounter with a passing star. One theory modeled the planet as originating in a disk close to the central binary, migrating inward to an unstable resonance with the binary, and then evolving rapidly to a highly eccentric orbit. The planet would be ejected unless its periastron distance was increased away from the binary, such as by a gravitational encounter with a passing star during apastron. An analysis of the motions of 461 nearby stars using Gaia observations revealed two that passed within of between 2 and 3 million years ago.
Public reaction
A petition had been launched asking the International Astronomical Union to name the companion Gallifrey, after the homeworld of The Doctor on the British science fiction series Doctor Who. The petition gathered over 139,000 signatures. In January 2014, however, it was agreed by the IAU not to accept the petition's goal to name it Gallifrey, as the petition did not follow the public policy of the IAU that a discussion between the public and IAU should be started before naming any spatial entity, and that this policy was not respected. In 2009, IAU stated that it had no plans to assign names to extrasolar planets, considering it impractical. However, in August 2013 the IAU changed its stance, inviting members of the public to suggest names for exoplanets.
