2006A&A...450.1221B -
Astronomy and Astrophysics, volume 450, 1221-1229 (2006/5-2)
Birth and fate of hot-Neptune planets.
BARAFFE I., ALIBERT Y., CHABRIER G. and BENZ W.
Abstract (from CDS):
This paper presents a consistent description of the formation and the subsequent evolution of gaseous planets, with special attention to short-period, low-mass hot-Neptune planets characteristic of µ Ara-like systems. We show that core accretion, including migration and disk evolution, and subsequent evolution, taking irradiation and evaporation into account, provides a viable formation mechanism for this type of strongly irradiated light planets. At an orbital distance due to the incident XUV stellar flux. In order to reach a µ Ara-like mass (∼14M⊕) after ∼1Gyr, the initial planet mass must range from 166M⊕ (∼0.52MJ) to about 20M⊕, for evaporation rates varying by 2 orders of magnitude, which corresponds to 90% to 20% mass loss during evolution. The presence of a core and heavy elements in the envelope affects the structure and the evolution of the planet appreciably and yields ∼8%-9% difference in radius compared to coreless objects of solar composition for Saturn-mass planets. These combinations of evaporation rates and internal compositions translate into different detection probabilities and thus into different statistical distributions for hot-Neptunes and hot-Jupiters. These calculations provide an observable diagnostic, namely a mass-radius-age relationship to distinguish between the present core-accretion-evaporation model and the alternative colliding core scenario for the formation of hot-Neptunes.
Abstract Copyright:
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Journal keyword(s):
planetary systems: formation - stars: individual: µ Ara
CDS comments:
Paragraph 3.1. HD 209548b is a misprint for HD 209458b. OGLE-TR 26b is a probable misprint for OGLE-TR 56b.
Simbad objects:
3
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