Abstract
The solar system consists of three different types of planets located in three distinctly separated areas. Their orbits are mostly circular and confined in a plane perpendicular to the sun’s rotation axis. These regular features have led to a standard scenario for the solar system formation through the collisional growth of small rocky and icy particles (planetesimals) and subsequent gas accretion within a rotating circumstellar disk of gas and dust (protoplanetary disk). Since then, a huge diversity of exoplanets, planets orbiting stars other than the sun, has been discovered. With the steady improvements in the observational technique and the advent of new tools, we are beginning to obtain detailed information on the architectures and physical properties of those distant new worlds. Such efforts have consequently revealed that the properties of our solar system may not be the norm, and called into question what we thought we knew about the solar system. One of the goals of exoplanetary science is to understand the diversity in orbital and physical properties in a comprehensive manner. More specifically, we wish to distinguish the features of planetary systems that necessarily result from the law of Nature, from those that are sculpted by accidents specific to each system. This thesis is to deal with one aspect of those “nature and nurture” problems in exoplanetary science, which will be described in the first three chapters.
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Notes
- 1.
- 2.
The two names are often used rather loosely without referring to their physical properties, as their internal structures are usually not very well constrained.
- 3.
At least they are not known, or confirmed, to exist; the predicted mass of “Planet Nine,” a hypothetical planet in the outer solar system, may be in this range (Batygin and Brown 2016).
- 4.
Strictly speaking, it is always possible that the object with \(M_\mathrm{p}\sin i\) comparable to that of Jupiter is actually a substellar object (e.g., Sahlmann et al. 2011). It should be noted, however, that the minimum mass is a priori close to the true mass if the orbit direction is isotropic; for example, the probability that the true mass is larger than the twice of the minimum mass is only \(13\%\), and the true mass is larger than the minimum mass only by a factor of \(4/\pi \) on average.
- 5.
We use Kepler’s third law divided by the stellar radii cubed, \(4\pi ^2(a/R_\star )^3/P^2=GM_\star /R_\star ^3\), to derive this scaling. The relation shows that the timescale of the transit essentially fixes the density of the system, which is the only physical dimension constrained from the light curve alone (see also Appendix B).
- 6.
- 7.
The letter “a” is reserved for the central star. If the host star forms a multi-stellar system, the capital letter follows after the Kepler number to specify the planet-hosting component (like “Kepler-16A b”). The order of planet letters is sometimes irregular because inner planets may be found after the outer one(s) in some cases.
- 8.
See, e.g., Sect. 9.2 of Weinberg (2008).
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Masuda, K. (2018). Diversity of the Extrasolar Worlds. In: Exploring the Architecture of Transiting Exoplanetary Systems with High-Precision Photometry. Springer Theses. Springer, Singapore. https://doi.org/10.1007/978-981-10-8453-9_1
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