Can we detect the stellar differential rotation of WASP-7 through the Rossiter–McLaughlin observations?

ABSTRACT The Rossiter–McLaughlin (RM) effect is the radial velocity signal generated when an object transits a rotating star. Stars rotate differentially and this affects the shape and amplitude of this signal, on a level that can no longer be ignored with precise spectrographs. Highly misaligned planets provide a unique opportunity to probe stellar differential rotation via the RM effect, as they cross several stellar latitudes. In this sense, WASP-7, and its hot Jupiter with a projected misalignment of ∼90°, is one of the most promising targets. The aim of this work is to understand if the stellar differential rotation is measurable through the RM signal for systems with a geometry similar to WASP-7. In this sense, we use a modified version of soap3.0 to explore the main hurdles that prevented the precise determination of the differential rotation of WASP-7. We also investigate whether the adoption of the next generation spectrographs, like ESPRESSO, would solve these issues. Additionally, we assess how instrumental and stellar noise influence this effect and the derived geometry of the system. We found that, for WASP-7, the white noise represents an important hurdle in the detection of the stellar differential rotation, and that a precision of at least 2 m s−1 or better is essential.

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Tidally induced stellar oscillations: converting modelled oscillations excited by hot Jupiters into observables

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3394 ◽

2020 ◽

Vol 500 (2) ◽

pp. 2711-2731

Author(s):

Andrew Bunting ◽

Caroline Terquem

Keyword(s):

Radial Velocity ◽

Orbital Period ◽

Planetary Systems ◽

Velocity Signal ◽

Convective Flux ◽

Hot Jupiters ◽

Stellar Oscillations ◽

Orbital Periods ◽

Hot Jupiter

ABSTRACT We calculate the conversion from non-adiabatic, non-radial oscillations tidally induced by a hot Jupiter on a star to observable spectroscopic and photometric signals. Models with both frozen convection and an approximation for a perturbation to the convective flux are discussed. Observables are calculated for some real planetary systems to give specific predictions. The photometric signal is predicted to be proportional to the inverse square of the orbital period, P−2, as in the equilibrium tide approximation. However, the radial velocity signal is predicted to be proportional to P−1, and is therefore much larger at long orbital periods than the signal corresponding to the equilibrium tide approximation, which is proportional to P−3. The prospects for detecting these oscillations and the implications for the detection and characterization of planets are discussed.

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Asteroseismology of exoplanet host stars

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316006219 ◽

2015 ◽

Vol 11 (A29B) ◽

pp. 620-627

Author(s):

Daniel Huber

Keyword(s):

Radial Velocity ◽

Planetary Systems ◽

Precise Determination ◽

Spin Orbit ◽

Velocity Measurements ◽

Fundamental Properties ◽

Future Space ◽

Host Stars

AbstractAsteroseismology is among the most powerful observational tools to determine fundamental properties of stars. Space-based photometry has recently enabled the systematic detection of oscillations in exoplanet host stars, allowing a combination of asteroseismology with transit and radial-velocity measurements to characterize planetary systems. In this contribution I will review the key synergies between asteroseismology and exoplanet science such as the precise determination of radii and ages of exoplanet host stars, as well as applications of asteroseismology to measure spin-orbit inclinations in multiplanet systems and orbital eccentricities of small planets. Finally I will give a brief outlook on asteroseismic studies of exoplanet hosts with current and future space-based missions such as K2 and TESS.

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Determination of Stellar Rotational Velocities

Symposium - International Astronomical Union ◽

10.1017/s0074180900078839 ◽

1985 ◽

Vol 111 ◽

pp. 163-184

Author(s):

Arne Slettebak

Keyword(s):

Radial Velocity ◽

Line Profile ◽

Binary Systems ◽

Profile Analysis ◽

Axial Rotation ◽

Line Profile Analysis ◽

Eclipsing Binary ◽

Rotating Star

The three basic methods for measuring axial rotation of stars had been suggested before the beginning of this century. These are (1) Modulation of starlight due to dark or bright areas on a rotating star; (2) Distortions in the radial velocity curves of eclipsing binary systems; and (3) Line profile analysis. Research in each of these areas is reviewed.

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NOESY around the critical point Omega Tau c = 1.12. Precise determination of proton-proton distances and reorientation correlation times with two-field NOESY

Molecular Physics ◽

10.1080/002689700162621 ◽

2000 ◽

Vol 98 (4) ◽

pp. 201-210

Author(s):

Tao Zhang, Xi-An Mao, Matthias Baur, Ho

Keyword(s):

Critical Point ◽

Precise Determination ◽

Correlation Times ◽

Proton Proton

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Precise determination of 14 REEs in GSJ/AIST geochemical reference materials JCp-1 (coral) and JCt-1 (giant clam) using isotope dilution ICP-quadrupole mass spectrometry

GEOCHEMICAL JOURNAL ◽

10.2343/geochemj.2.0498 ◽

2018 ◽

Vol 52 (1) ◽

pp. 75-79 ◽

Cited By ~ 2

Author(s):

Tsuyoshi Tanaka ◽

Seung-Gu Lee ◽

Taehoon Kim ◽

Seunghee Han ◽

Hyo Min Lee ◽

...

Keyword(s):

Mass Spectrometry ◽

Reference Materials ◽

Isotope Dilution ◽

Precise Determination ◽

Giant Clam ◽

Quadrupole Mass ◽

Quadrupole Mass Spectrometry ◽

Geochemical Reference Materials

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PRECISE DETERMINATION OF THE IRRATIONAL PRE-FERRED INTERFACE ORIENTATION BY TEM

ACTA METALLURGICA SINICA ◽

10.3724/sp.j.1037.2010.00411 ◽

2010 ◽

Vol 46 (4) ◽

pp. 411-417 ◽

Cited By ~ 4

Author(s):

Yang MENG ◽

Lin GU ◽

Wenzheng ZHANG

Keyword(s):

Precise Determination ◽

Interface Orientation

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Nauwkeurige methode voor de aanwasbepaling van het grondvlak met behulp van de Pressler-boor

Silva Gandavensis ◽

10.21825/sg.v12i0.1009 ◽

1968 ◽

Vol 12 ◽

Author(s):

R. Goossens

Keyword(s):

Basal Area ◽

Precise Determination ◽

Maximum Diameter ◽

Precise Method ◽

Maximum Radius ◽

The Core ◽

Two Parameters

A precise method for the determination of the increment of the basal area using the PressIer bore. Refering to previous research showing that the basal area of the corsica pine could be characterized by an ellips, we present in this paper a precise method for the determination of the increment of the basal area. In this method we determine the direction of the maximum diameter, we measure this diameter and we take a core in one of the points of tangency of the caliper with the measured tree. The determination of the diameter perpendicular to the maximum diameter finishes the work wich is to be done in the forest. From the classical measurements effectuated on the core and from the measured diameters we can then determine the form (V) and the excentricity (e). Substituting these two parameters in the formula 2 or 2', we can also calculate the error of a radius measured on the core with respect to the representative radius, This error with them allow us to correct the measured value of the minimum or the maximum radius and we will be able to do a precise determination of the increment.

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