TIDAL HEATING MODELS FOR THE RADII OF THE INFLATED TRANSITING GIANT PLANETS WASP-4b, WASP-6b, WASP-12b, WASP-15b, AND TrES-4
TIDAL HEATING MODELS FOR THE RADII OF THE INFLATED TRANSITING GIANT PLANETS WASP-4b, WASP-6b, WASP-12b, WASP-15b, AND TrES-4
复制标题
膨胀凌日巨行星 WASP-4b、WASP-6b、WASP-12b、WASP-15b 和 TrES-4 半径的潮汐加热模型
DOI：
10.1088/0004-637x/713/2/751
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发表时间：
2009
期刊：
影响因子：
--
通讯作者：
D. Spiegel
中科院分区：
文献类型：
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作者：
L. Ibgui;A. Burrows;D. Spiegel
为了解释一些凌日系外巨行星的膨胀半径，我们研究了膨胀行星WASP-4 b，WASP-6 b，WASP-12 b，WASP-15 b和TrES-4的潮汐加热方案。为此，我们假设它们保持非零的离心率，可能是由于与第三个物体的持续相互作用。我们计算的额外热量的信封，然后需要适合每个行星的半径，我们探讨如何这种额外的权力取决于行星大气的不透明度和重元素的中央核心的质量。在核心质量Mcore和加热之间存在简并。因此，在潮汐加热的情况下，每个行星都有一个{Mcore，e2/Q′p}的范围，可以导致相同的半径，其中Q′p是潮汐耗散因子，e是离心率。考虑到这一点，我们还调查了非膨胀行星HAT-P-12 b的情况，它可以承认结合重元素核心和潮汐加热的解决方案。对这类行星系统的测量偏心率的实质性改进可以通过将两个未知参数{Mcore，Q′p}联系起来来简化这种简并。通过我们的计算，对这两个参数中任何一个的进一步独立约束都会约束另一个。
In order to explain the inflated radii of some transiting extrasolar giant planets, we investigate a tidal heating scenario for the inflated planets WASP-4b, WASP-6b, WASP-12b, WASP-15b, and TrES-4. To do so, we assume that they retain a nonzero eccentricity, possibly by dint of continuing interaction with a third body. We calculate the amount of extra heating in the envelope that is then required to fit the radius of each planet, and we explore how this additional power depends on the planetary atmospheric opacity and on the mass of a heavy-element central core. There is a degeneracy between the core mass Mcore and the heating . Therefore, in the case of tidal heating, there is for each planet a range of {Mcore, e2/Q′p} that can lead to the same radius, where Q′p is the tidal dissipation factor and e is the eccentricity. With this in mind, we also investigate the case of the non-inflated planet HAT-P-12b, which can admit solutions combining a heavy-element core and tidal heating. A substantial improvement of the measured eccentricities of such planetary systems could simplify this degeneracy by linking the two unknown parameters {Mcore, Q′p}. Further independent constraints on either of these parameters would, through our calculations, constrain the other.
DOI：
10.1088/0004-637x/709/1/159
发表时间：
2009-08
期刊：
The Astrophysical Journal
影响因子：
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作者：
D. Anderson;C. Hellier;M. Gillon;M. Gillon;A. Triaud;B. Smalley;L. Hebb;A. Cameron;P. Maxted;D. Queloz;R. West;S. Bentley;B. Enoch;K. Horne;T. Lister;M. Mayor;N. Parley;F. Pepe;D. Pollacco;D. Ségransan;S. Udry;D. Wilson;D. Wilson
通讯作者：
D. Anderson;C. Hellier;M. Gillon;M. Gillon;A. Triaud;B. Smalley;L. Hebb;A. Cameron;P. Maxted;D. Queloz;R. West;S. Bentley;B. Enoch;K. Horne;T. Lister;M. Mayor;N. Parley;F. Pepe;D. Pollacco;D. Ségransan;S. Udry;D. Wilson;D. Wilson