HD 149026 b

Planetbox begin
name = HD 149026 bPlanetbox star
star = HD 149026
constell = Hercules
RA = RA|16|30|29.619
DEC = DEC|+38|20|50.31
dist_ly = 257
dist_pc = 78.9 ± 6.6
class = G0IVPlanetbox orbit
position_angle =
semimajor = 0.042
eccentricity = 0
period = 2.8758882 ± 0.0000061
inclination =
ang_dist =
long_peri =
arg_peri =
t_peri = 2,453,530.751
t_transit =
t_approach =
semi-amp = 43.2 ± 2.6Planetbox character
mass = 0.36 ± 0.03
radius = 0.725 ± 0.03
density = 1252
gravity =
temperature = 2300 ± 200Planetbox discovery
discovery_date = 1 July 2005
discoverers = B. Sato,
D. Fischer,
G. Henry "et al."
discovery_method = Radial velocity
discovery_site = flag|United States
discovery_status = Confirmed

HD 149026 b is an extrasolar planet approximately 257 light-years away in the constellation of Hercules. The planet was discovered after it transited its parent star, HD 149026. It is notable for the presence of an exceptionally large planetary core suggested by measurements of its radius and mass.

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. cite journal | author=Sato "et al." | title=The N2K Consortium. II. A Transiting Hot Saturn around HD 149026 with a Large Dense Core | journal=The Astrophysical Journal | year=2005 | volume=633 | issue=1 | pages=465 – 473 | url=http://www.journals.uchicago.edu/doi/full/10.1086/449306 | doi=10.1086/449306 ]

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. cite news | first=Robert | last=Naeye | pages= | title=Amateur Detects New Transiting Exoplanet | date=July 7, 2005 | publisher=Sky & Telescope | url=http://skyandtelescope.com/news/article_1543_1.asp ]

Physical characteristics

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 on the basis of 0.3 Bond albedo to be about 1540 K, above the predicted temperature of HD 209458 b (1400K) which had inaugurated the category of Chthonian "hell planet". [ [http://www.bioedonline.org/news/news.cfm?art=777 Hell planet gets solar hammering] ] 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 is around the boiling point of silicon and well above the melting point of iron.

This planet's albedo has not been measured directly. The initial estimate of 0.3 had come from averaging Sudarsky's theoretical classes IV and V. The planet's extremely high temperature has forced astronomers to abandon that estimate; now, they predict that the planet must absorb essentially all of the starlight that falls on it - that is, effectively zero albedo like HD 209458 b. [ [http://spaceflightnow.com/news/n0705/09hotplanet/ Spaceflight Now | Breaking News | Exotic extrasolar planet is the hottest yet discovered ] ] Much of the absorption takes place at the top of its atmosphere; between that and the hot, high pressure gas surrounding the core, a stratosphere of cooler gas is predicted. [Cite arXiv| author=Ivan Hubeny, Adam Burrows |title=Spectrum and atmosphere models of irradiated transiting extrasolar giant planets |eprint=0807.3588v1| class=astro-ph|year=2008] The outer shell of dark, opaque, hot clouds are usually thought to be vanadium and titanium oxides ("pM planets"), but other compounds like tholins cannot be ruled out as yet.

The planet-star radius ratio is 0.05158 +/- 0.00077. [Cite arXiv|author=Nutzman, Philip "et al."|title=A Precise Estimate of the Radius of HD 149026b|eprint=0807.1318|class=astro-ph|year=2008] Currently what limits more precision on HD 149026 b's radius "is the uncertainty in the stellar radius",cite journal | url=http://schwab.tsuniv.edu/papers/apj/hd149026_3/reprint.pdf| journal=The Astrophysical Journal| author=Joshua N. Winn "et al."| title=Five New Transits of the Super-Neptune HD 149026b| volume=675| pages=1531–1537| year=2008| month=March |doi=10.1086/527032] and measurement of the stellar radius is distorted by pollution on the star's surface. [cite arXiv | title=Extent of pollution in planet-bearing stars | author=S.-L. Li, D. N. C. Lin, and X.-W. Liu |class=astro-ph | year=2008 |eprint=0802.2359v1]

Even allowing for uncertainty the radius of HD 149026 b is only about three quarters that of Jupiter (or 83% that of Saturn). Only Gliese 436 b of 52 planets known to transit their stars as of August 2008 is smaller in radius than HD 149026 b.

There are a number of such "hot Saturns", but HD 149026 b is so far unique: HD 149026 b's low volume means that the planet is unexpectedly dense for a gas giant of its mass and temperature. It may have an exceptionally large core composed of elements heavier than hydrogen and helium: the initial theoretical models gave the core a mass of 70 times Earth's mass; further refinements suggest 80-110 Earth masses. [cite arXiv | title=POSSIBLE SOLUTIONS TO THE RADIUS ANOMALIES OF TRANSITING GIANT PLANETS |author=A. Burrows, I. Hubeny, J. Budaj, & W.B. Hubbard | class=astro-ph | year=2007 | eprint=0612703v2] As a result, the planet has been described as a "super-Neptune", in analogy to the core-dominated outer ice giants of our solar system, though whether the core of HD 149026 b is mainly icy or rocky is not currently known. Robert Naeye in "Sky & Telescope" claimed "it contains as much or more heavy elements (elements heavier than hydrogen and helium) than all the planets and asteroids in our solar system combined". [http://skyandtelescope.com/news/article_1538_1.asp One Big Ball of Rock] Robert Naeye, Sky & Telescope, last accessed October 13, 2007] In addition to uncertainties of radius, its tidal heating over its history needs be taken into account; if its current orbit had evolved from a more eccentric one, the extra heat increases its expected radius per its model and thereby its core radius. [Cite arXiv| author=Brian Jackson, Richard Greenberg, Rory Barnes| title=Tidal Heating of Extra-Solar Planets |eprint=0803.0026v1 |class=astro-ph|year=2008]

Naeye further speculated that the gravity could be as high as ten "g" (ten times gravity on Earth's surface) on the surface of the core.

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.

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.

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. cite journal | author=Wolf, A. S.; Laughlin, G.; Henry, G. W., Fischer, D. A.; Marcy, G.; Butler, P.; Vogt, S. | title=A Determination of the Spin-Orbit Alignment of the Anomalously Dense Planet Orbiting HD 149026 | journal=The Astrophysical Journal | year=2007 | volume=667 | issue=1 | pages= 549–556 | url=http://www.journals.uchicago.edu/doi/abs/10.1086/503354 | doi=10.1086/503354( [http://www.oklo.org/HD149026.pdf preprint] )] As of August 2008 this is still the canonical measurement. [cite arXiv | title= Measuring accurate transit parameters | author=Joshua N. Winn | eprint=0807.4929v2 |class=astro-ph |year=2008]

See also

* HAT-P-3b
* HD 209458 b
* HD 179949 b
* Tau Boötis b

References

External links

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