HD 106906 b

HD 106906 b

The star HD 106906 and the planet HD 106906 b, with Neptune's orbit for comparison
Discovery
Discovered by	Vanessa Bailey, et al.
Discovery site	Magellan Telescopes at the Las Campanas Observatory in Chile
Discovery date	December 4, 2013 (published)
Detection method	Direct imaging
Orbital characteristics
Mean orbit radius	738 AU (110 billion km)
Orbital period (sidereal)	8,910.501 years
Star	HD 106906
Physical characteristics
Mean radius	1.54+0.04 −0.05 RJ
Mass	11±2 MJup
Temperature	≈1,800 K (1,500 °C; 2,800 °F)

HD 106906 b is a directly imaged planetary-mass companion and exoplanet orbiting the star HD 106906, in the constellation Crux at about 336 ± 13 light-years (103 ± 4 pc) 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. HD 106906 b is an oddity; 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

HD 106906 b is the only known companion orbiting HD 106906, a spectroscopic binary star composed of two F5V main-sequence stars with a combined mass of 2.71 M_☉. Based on the star's luminosity and temperature, the system is estimated to be about 13±2 million years old. The system is a likely member of the Scorpius–Centaurus association. The star is surrounded by a debris disk oriented 21 degrees away from HD 106906 b; this disk is about 65 AU (10 billion km; 6 billion mi) from the binary on its interior and ranges asymmetrically from approximately 120 to 550 AU (18 to 82 billion km; 11 to 51 billion mi) from the binary at its outer edge. Based on its near-infrared spectral-energy distribution, its age, and relevant evolutionary models, HD 106906 b is estimated to be 11±2 M_Jup, with a surface temperature of 1,800 K (1,500 °C; 2,800 °F). A spectrum with Magellan does show a spectral type of L2.5 ±1 and intermediate gravity. A high-signal-to-noise spectrum was taken with VLT/SINFONI, which resulted in a spectral type of L1.5 ± 1.0 and a temperature of 1820 ± 240 K. Depending on its formation it has a mass of 11.9+1.7
−0.8 M_J (hot start) or 14.0+0.2
−0.5 M_J (cold start). 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 beta Pictoris b or 1RXS J160929.1−210524 b, its projected separation from the star is much larger, about 738 AU (110 billion km; 69 billion mi), 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 HD 106906 b's Hill sphere at periastron.

The discovery team evaluated the possibility that HD 106906 b is not gravitationally bound to HD 106906, 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 HD 106906 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 HD 106906 A 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 HD 106906 b 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 HD 106906 b's 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 HD 106906 b, 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 (HIP 59716 and HIP 59721, a possible loosely bound binary system) that passed within 1 pc (3.3 ly) of HD 106906 between 2 and 3 million years ago.

Using archival spectral data a team found a C/O=0.53+0.15
−0.25 for HD 106906 b, consistent with the stellar association its host star formed in. This is consistent with stellar-like formation for the companion. This makes it unlikely that it formed like a planet in a disk around the binary.

Public reaction

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.

A petition had been launched asking the International Astronomical Union (IAU) 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.

Recent observations made by the Hubble Space Telescope strengthened the case for the planet having an unusual orbit that perturbed it from its host star's debris disk. NASA and several news outlets compared it to the hypothetical Planet Nine.

See also

• DT Virginis, a planetary mass object which orbits a binary star, it has the farthest known orbit of a known circumbinary object
• GU Piscium b, an exoplanet orbiting GU Piscium at a distance of 2000 AU and period of 80,000 years in the AB Doradus moving group
• Gliese 900 b, a planetary mass object with the widest discovered orbit
• Planet Nine, a hypothetical ninth planet in the outer region of the Solar System with similar wide semi-major axis of 460⁺¹⁶⁰
  ₋₁₀₀ AU