By Teruyuki Hirano
This thesis provides actual analyses of the spin-orbit attitude for plenty of striking transiting exoplanetary platforms, together with the 1st dimension of the Rossiter-McLaughlin influence for a a number of transiting system.
The writer provides the observational equipment had to probe the spin-orbit perspective, the relation among the stellar spin axis and planetary orbital axis. Measurements of the spin-orbit perspective supply us a distinct and necessary chance to appreciate the starting place of close-in enormous exoplanets, known as "hot Jupiters".
The first approach brought includes observations of the Rossiter-McLaughlin impact (RM effect). the writer issues out the problems with the former theoretical modeling of the RM impression and derives a brand new and stronger concept. purposes of the recent conception to observational information also are awarded for a couple of amazing structures, and the writer exhibits that the recent idea minimizes the systematic mistakes via utilizing it to the observational data.
The writer additionally describes one other strategy for constraining the spin-orbit attitude: by way of combining the measurements of stellar flux adaptations as a result of darkish spots at the stellar floor, with the projected stellar rotational speed measured through spectroscopy, the spin-orbit angles "along the line-of-sight" are restricted for the transiting exoplanetary platforms suggested via the Kepler house telescope.
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Extra info for Measurements of Spin-Orbit Angles for Transiting Systems: Toward an Understanding of the Migration History of Exoplanets
Sample text
These parameters are related to individual stellar properties such as the effective temperature, surface gravity, and the nature of each absorption line. Some line profiles of especially strong absorption lines (such as the Na D lines) are saturated and intrinsically different from the Voigt function in shape. However, most of the lines in the wavelength region used in RV analyses are relatively weak, by design, and are well approximated by the Voigt function in the absence of the stellar rotation and macroturbulence.
The template spectrum in this case is a box-shaped numerical mask. This means that in the presence of a line the mask function B takes unity, and in the absence of lines B takes zero. 2 0 5393 5394 5395 5396 5397 5398 5399 5400 5401 0 -30 -20 -10 wavelength [angstrom] 0 10 RV -1 velocity [km s ] 20 30 Fig. 2 Left A schematic plot of an observed spectrum (red) and the numerical mask at the bottom (blue). 1 for clarity. Right The cross-correlation function between the two spectra in the left panel (one observed and one theoretical).
1] further investigated this point and estimated the typical timescales for the stellar spin axis to “realign” with the planetary orbit based on the empirical equations for the tidal interaction by Zahn [23]. 9 indicates the “relative” timescale ζ needed for a spin-orbit realignment for each of the systems with RM measurements, estimated by the mass and orbit of the planet along with host star’s property. Although these timescales for the spin-orbit realignment were computed by simple relations originally derived for binary star systems, the result points to a trend; the longer ζ is, the more likely we observe a spin-orbit misalignment.
