scholarly journals KEPLER PLANETARY SYSTEMS: DOPPLER BEAMING EFFECT SIGNIFICANCE

2021 ◽  
Vol 57 (1) ◽  
pp. 123-132
Author(s):  
H. Barbier ◽  
E. López
Keyword(s):  
Light Curve ◽  
Radial Velocity ◽  
Observational Data ◽  
Close Agreement ◽  
Extrasolar Planets ◽  
Planetary Systems ◽  
Light Curves ◽  
Third Harmonic ◽  
Good Agreement

In the present work, in order to estimate the semi-amplitude of the radial velocity, we evaluate the contribution of the Doppler beaming effect to the phase curves of the all confirmed extrasolar planets (2776, September 2019), observed so far by the Kepler telescope. By modeling the tiny photometric variations (reflection, ellipsoidal and Doppler beaming effects) of the light curves, we found that the best observational data are in close agreement with the theoretical and published values of the amplitudes only for exoplanets: KOI-13b and TrES-2b. The derived values for the radial velocity also are in good agreement with those published by some authors. Furthermore, we found it necessary to introduce a third harmonic (3Φ) contribution into the KOI-13b and HAT-P7b light curve models, in order to decrease the residuals.

scholarly journals Extrasolar planet detections with gravitational microlensing

2007 ◽  
Vol 3 (S249) ◽  
pp. 25-30
Author(s):  
Shude Mao ◽  
Eamonn Kerins ◽  
Nicholas J. Rattenbury
Keyword(s):  
Light Curve ◽  
Real Time ◽  
Extrasolar Planets ◽  
Light Curves ◽  
Extrasolar Planet ◽  
Galactic Centre ◽  
Wide Field ◽  
High Magnification ◽  
Gravitational Microlensing

AbstractMicrolensing light curves due to single stars are symmetric and typically last for a month. So far about 4000 microlensing events have been discovered in real-time, the vast majority toward the Galactic centre. The presence of planets around the primary lenses induces deviations in the usual light curve which lasts from hours (for an Earth-mass [M⊕] planet) to days (for a Jupiter-mass [Mj] planet). Currently the survey teams, OGLE and MOA, discover and announce microlensing events in real-time, and follow-up teams (together with the survey teams) monitor selected events intensively (usually with high magnification) in order to identify anomalies caused by planets. So far four extrasolar planets have been discovered using the microlensing technique, with half a dozen new planet candidates identified in 2007 (yet to be published). Future possibilities include a network of wide-field 2m-class telescopes from the ground (which can combine survey and follow-up in the same setup) and a 1m-class survey telescope from space.

scholarly journals Analysis of the light and radial velocity curves of transiting extra-solar planets

2008 ◽  
Vol 4 (S253) ◽  
pp. 394-397
Author(s):  
Alvaro Giménez
Keyword(s):  
Light Curve ◽  
Radial Velocity ◽  
Light Curves ◽  
Approximate Algorithms ◽  
System Parameters ◽  
Main System ◽  
Analytical Expressions ◽  
Synthetic Models ◽  
Insight Into ◽  
Complete Solutions

AbstractSeveral approaches have been followed for the analysis of the light curves of transiting extra-solar planets. From simple approximate algorithms and synthetic models to semi-analytical complete solutions. The different alternatives are discussed with their strengths and weaknesses. Analytical expressions can also provide a deeper insight into the main system parameters from the measurement of a few strategic points describing the shape of the light curve.

scholarly journals OJ 287: A Blazar with Everything

1994 ◽  
Vol 159 ◽  
pp. 409-409
Author(s):  
L.O. Takalo
Keyword(s):  
Correlation Analysis ◽  
Light Curve ◽  
Observational Data ◽  
Light Curves ◽  
Simple Correlation ◽  
Data Set ◽  
Preliminary Results ◽  
Blazar Oj 287

We have collected all the observations available to us of blazar OJ 287. Here we will present preliminary results from our investigation of these data. The photometric light curves show large outbursts occuring (quasi)simultaneously in all frequences. The largest outbursts occured during 1972 and 1983. The B-band light curve can be extended to the year 1894. This being the longest available observational data set of all blazars. Polarization light curves in optical show random variations in all timescales. In the radio bands the polarization observations show well defined structure in the light curves. Light curves and simple correlation analysis based on the light curves on different frequences will be presented.

scholarly journals How to use the Phoebe code to solve transiting exoplanet light curve

2008 ◽  
Vol 4 (S253) ◽  
pp. 398-401
Author(s):  
Stanislav Poddaný
Keyword(s):  
Light Curve ◽  
Light Curves ◽  
Good Agreement

AbstractA brief demonstration of photometric light curves solutions for eight transiting exoplanets using the Phoebe 0.29c code is presented. We determined radii and inclinations for TrES-1b, TrES-2b, Wasp-1b, XO-1b, XO-2b, OGLE-TR-10b, OGLE-TR-111b and HD 189733b. All our results are in good agreement with the last results published.

scholarly journals Results from Microlensing Searches for Extrasolar Planets

2004 ◽  
Vol 202 ◽  
pp. 44-51 ◽  
Author(s):  
Penny D. Sackett
Keyword(s):  
Radial Velocity ◽  
Extrasolar Planets ◽  
Planetary Systems ◽  
Future Prospects ◽  
Subsequent Evolution

Specially-designed microlensing searches, some of which have been underway for several years, are sensitive to extrasolar planets orbiting the most common stars in our Galaxy. Microlensing is particularly well-suited to the detection of Jupiter-mass planets orbiting their parent stars at several AU. Since Jovian analogs are thought to influence the subsequent evolution of most planetary systems, they are particularly important to study. The orbital radii and distances to the planetary systems probed by microlensing are larger than those currently studied by radial velocity techniques; the two methods are thus complementary. Recent results from microlensing searches are discussed, including constraints on Jovian analogs orbiting typical Galactic stars. Benefits and drawbacks of the technique for the characterization of planetary systems, and future prospects are briefly reviewed.

scholarly journals New Insights into the Dynamics of Planets in P-Type Motion Around Binaries

2011 ◽  
Vol 7 (S282) ◽  
pp. 446-447
Author(s):  
Barbara Funk ◽  
Siegfried Eggl ◽  
Markus Gyergyovits ◽  
Richard Schwarz ◽  
Elke Pilat-Lohinger
Keyword(s):  
Observational Data ◽  
Extrasolar Planets ◽  
Giant Planet ◽  
Planetary Systems ◽  
Large Percentage ◽  
Stellar Systems ◽  
Extrasolar Systems ◽  
Different Types ◽  
M Stars ◽  
P Type

AbstractUp to now, more than 500 extra-solar planets have been discovered. Many of these extrasolar systems consist of one star and only one giant planet. However, recently more and more different types of systems have become known, including also extrasolar planets in binaries. In our study, we will concentrate on such systems, since a large percentage of all G-M stars are expected to be part of binary or multiple stellar systems. Therefore, these kinds of systems are worthy of investigation in detail. In particular, we will concentrate on planets in P-Type motion, where the planet orbits around both stars. During the last few years, four such systems (NN Ser, HW Vir, HU Aqr and DP Leo) have been discovered. In our study, we performed dynamical studies for three multi-planetary systems in binaries (NN Ser, HW Vir, HU Aqr), and compared simulated eclipse timing variations (ETV) to current observational data.

scholarly journals Higher order harmonics in the light curves of eccentric planetary systems

2019 ◽  
Vol 488 (3) ◽  
pp. 4181-4194 ◽  
Author(s):  
Zephyr Penoyre ◽  
Emily Sandford
Keyword(s):  
Light Curve ◽  
Planetary Systems ◽  
Higher Order ◽  
Photometric Data ◽  
Light Curves ◽  
Combined Effects ◽  
Eccentric Orbits ◽  
Relativistic Beaming ◽  
Orbital Frequency ◽  
Reflection Of Light

ABSTRACTAs a planet orbits, it causes periodic modulations in the light curve of its host star. Due to the combined effects of the planet raising tides on the host star, relativistic beaming of the starlight, and reflection of light off the planet’s surface, these modulations occur at the planet’s orbital frequency, as well as integer multiples of this frequency. In particular, planets on eccentric orbits induce third and higher order harmonics in the stellar light curve which cannot be explained by circular-orbit models. Even at moderate eccentricities, such as those typical of Solar system planets, these harmonics are detectable in current and future photometric data. We present an analysis of the harmonics caused by tides, beaming, and reflection in eccentric planetary systems. We explore the dependence of these signals on the parameters of the system, and we discuss prospects for current and future observations of these signals, particularly by the NASA TESS mission. Finally, we present publicly available code for computation of light curves with tidal, beaming, and reflection signals, oot.

scholarly journals TESS exoplanet candidates validated with HARPS archival data

2019 ◽  
Vol 622 ◽  
pp. L7 ◽  
Author(s):  
Trifon Trifonov ◽  
Jan Rybizki ◽  
Martin Kürster
Keyword(s):  
Light Curve ◽  
Radial Velocity ◽  
Planetary Systems ◽  
Archival Data ◽  
Velocity Analysis ◽  
Orbital Parameters ◽  
Mean Motion ◽  
Two Systems ◽  
Made In ◽  
Mean Motion Resonance

Aims. We aim at the discovery of new planetary systems by exploiting the transit light-curve results from observations made in TESS orbital observatory Sectors 1 and 2 and validating them with precise Doppler measurements obtained from archival HARPS data. Methods. Taking advantage of the reported TESS transit events around GJ 143 (TOI 186) and HD 23472 (TOI 174), we modeled their HARPS precise Doppler measurements and derived orbital parameters for these two systems. Results. For the GJ 143 system, TESS has reported only a single transit, and thus its period is unconstrained from photometry. Our radial velocity analysis of GJ 143 reveals the full Keplerian solution of the system, which is consistent with an eccentric planet with a mass almost twice that of Neptune and a period of Pb = 35.59−0.1+0.1 days. Our estimates of the GJ 143 b planet are fully consistent with the transit timing from TESS. We confirm the two-planet system around HD 23472, which according to our analysis is composed of two Neptune-mass planets in a possible 5:3 mean motion resonance.

scholarly journals Several problems of exoplanetary orbits determination from radial velocity observations

2007 ◽  
Vol 3 (S249) ◽  
pp. 101-110 ◽  
Author(s):  
Roman V. Baluev
Keyword(s):  
Time Series ◽  
Radial Velocity ◽  
Extrasolar Planets ◽  
Planetary Systems ◽  
Systematic Errors ◽  
Giant Planets ◽  
Dwarf Star ◽  
Statistical Bias ◽  
Outer Planets

AbstractExisting algorithms of analysis of radial velocity time series are improved for the purposes of extrasolar planets detection and characterizing. Three important effects are considered: the poorly known radial velocity jitter, periodic systematic errors, and statistical bias due to non-linearity of models. Mathematical tools to account for these effects are developed and applied to a number of real planetary systems. In particular, it is shown that two outer planets of HD37124 are likely trapped in the 2/1 resonance. The dwarf star GJ876 may host an extra, Neptune-mass, planet which is in resonance with two giant planets in this system.

scholarly journals BEER analysis of Kepler and CoRoT light curves – V. eBEER: extension of the algorithm to eccentric binaries

2020 ◽  
Vol 497 (4) ◽  
pp. 4884-4895
Author(s):  
M Engel ◽  
S Faigler ◽  
S Shahaf ◽  
T Mazeh
Keyword(s):  
Light Curve ◽  
Radial Velocity ◽  
Binary Systems ◽  
Light Curves ◽  
Harmonic Series ◽  
Eclipsing Binary ◽  
Fast Processing

ABSTRACT We present an extension of the BEER model for eccentric binaries – eBEER, approximating the BEaming, Ellipsoidal, and Reflection effects by harmonic series of the Keplerian elements of their orbit. As such, it can be a tool for fast processing of light curves for detecting non-eclipsing eccentric binary systems. To validate the applicability of the eccentric model and its approximations, we applied eBEER to the Kepler light curves, identified a sample of bright non-eclipsing binary candidates, and followed three of them with the Wise observatory eShel spectrograph. After confirming the three systems are indeed radial velocity (RV) binaries, we fitted the light curves and the RV data with PHOEBE, a detailed numerical light curve and RV model, and showed that the PHOEBE derived parameters are similar to those obtained by the eBEER approximation.

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