HD 149026 b

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**HD 149026 b**
Discovery
HD 149026 b (artist's conception)
Discovered by	B. Sato, D. Fischer, G. Henry et al.
Discovery site	Keck and Subaru telescopes
Discovery date	July 1, 2005
Detection method	Radial velocity
Orbital characteristics
Semi-major axis	0.042 AU
Eccentricity	(fixed) 0
Orbital period	2.8758882 ± 0.0000061 d ^[1]
Longitude of periastron	-
Time of periastron	2,453,530.751 (transit time) JD
Semi-amplitude	43.2 ± 2.6 m/s
Physical characteristics
Mean radius	0.725 ± 0.03 R_J
Mass	0.36 ± 0.03 M_J
Temperature	2300 ± 200 K^[2]

HD 149026 b, is a transiting extrasolar planet orbiting the star HD 149026. It is notable for the presence of an exceptionally large planetary core suggested by measurements of its radius and mass.

1 Discovery
2 Characteristics
3 Theoretical consequences
4 See also
5 References
6 External links

[edit] Discovery

The planet was discovered by the N2K Consortium in 2005, which searches stars for closely orbiting giant planets similar to 51 Pegasi b using the highly successful radial velocity method. The spectrum of the star was studied from the Keck and Subaru Telescopes. After the planet was first detected from the Doppler effect it caused in the light of the host star, it was studied for transits at the Fairborn Observatory. A tiny decrease of light (0.003 magnitudes) was detected every time the planet was transiting the star, thus confirming its existence. ^[3]

Although the change of brightness caused by the transiting planet is tiny, it is detectable by amateur astronomers, providing an opportunity for amateurs to make important astronomical contributions. Indeed, one amateur astronomer, Ron Bissinger, actually detected a partial transit a day before the discovery was published. ^[4]

[edit] Characteristics

Comparison of the inner core of the extrasolar planet HD 149026b and Jupiter

The planet orbits the star in a so-called "torch orbit". One revolution around the star takes only a little less than three Earth days to complete. The planet is less massive than Jupiter (0.36 times Jupiter's mass, or 114 times Earth's mass) but more massive than Saturn. The temperature of the planet was initially estimated to be about 1540 K based on a reasonable albedo value of 0.3, making the planet a borderline case between the Class IV and Class V planets in the Sudarsky classification scheme.^[3] Its day-side brightness temperature was subsequently directly measured as 2,300 ± 200 K by comparing the combined emissions of star and planet at 8 μm wavelength before and during a transit event. This extremely high temperature indicates that the planet must absorb essentially all of the starlight that falls on it, making it unusually dark in color.^[2]^[5]

There are a number of such "hot Saturns", but HD 149026 b is so far unique. It has been described as a "hell planet", being charcoal black in color and a burnt magma hue in starlight^{[citation needed]}. Surface temperatures are above the boiling point of lead. Most transiting planets have radii comparable to Jupiter's or more; however, the radius of HD 149026 b is only about 73% that of Jupiter (or 83% that of Saturn), meaning that the planet is unexpectedly dense for a gas giant of its mass. It may have an exceptionally large core composed of elements heavier than hydrogen and helium.^[3] Theoretical models give the core a mass of 70 times Earth's mass. In fact, the planet may have more rocky^{[citation needed]} and metallic material^{[citation needed]} than all the planets in our Solar system combined.^{[citation needed]}

Robert Naeye speculated that the gravity could be as high as ten g (ten times gravity on Earth's surface) on the surface of the core.^[6]

[edit] Theoretical consequences

The discovery was advocated as a piece of evidence for the popular solar nebula accretion model, where planets are formed from the accretion of smaller objects. In this model, giant planet embryos grow large enough to acquire large envelopes of hydrogen and helium. However, opponents of this model emphasize that only one example of such dense planet is not a proof. In fact, such a huge core is difficult to explain even by the core accretion model. ^[3]

One possibility is that because the planet orbits so close to its star, it is — unlike Jupiter — ineffective in cleansing the planetary system of rocky bodies. Instead, a heavy rain of heavier elements on the planet may have helped creating the large core. ^[3]

Careful radial velocity measurements have made it possible to detect the Rossiter-McLaughlin effect, the shifting in photospheric spectral lines caused by the planet occulting a part of the rotating stellar surface. This effect allows the measurement of the angle between the planet's orbital plane and the equatorial plane of the star. In the case of HD 149026 b, the alignment was measured to be +11° ± 14°. This in turn suggests that the formation of the planet was peaceful and probably involved interactions with the protoplanetary disc. A much larger angle would have suggested a violent interplay with other protoplanets. ^[7]