Extremely Inflated Hot Jupiters Could Be Extremely Young

Details Extremely Inflated Hot Jupiters Could Be Extremely Young Extremely Inflated Hot Jupiters Could Be Extremely Young

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.4301m&link_type=abstract

American Astronomical Society, ESS meeting #2, #43.01

Astronomy and Astrophysics

Astronomy

Scientific paper

Extremely inflated hot Jupiters could have formed recently from the merger of two low-mass stars.
The frequency of W UMa stars is not enough
to account for many inflated hot Jupiters,
so low mass detached binaries could also contribute to the progenitor population.
We find that the degree of inflation of the transiting hot Jupiters correlates with their expected spiral-in life time by tidal dissipation, and this
could be an indication of youth if the Q dissipation parameter is sufficiently low, as suggested by the
studies of the Jupiter-Io system.
There is also a correlation between radius anomaly and host star rotational velocity as expected in the merger scenario.
The distribution of rotational velocities among the host stars is statistically similar to that of blue
stragglers in the globular cluster 47 Tuc. A significant challenge to the binary merger hypothesis
is the efficient angular momentum loss required to explain the slow rotation of some inflated hot Jupiter host stars.
As observational tests we point out that if hot Jupiters are mainly formed as a result of binary mergers, the frequency of this kind of planets should be higher around blue stragglers than around T Tauri stars.
The presenter is supported by funding
from the Spanish Ministry of Science
and Technology and the ROPACS european
training network.

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