Introduction
... years1 away, the planet appears very close to its star and its faint light is diluted in the glare of its star. Indirect methods designed to detect an exoplanet through its influence on its parent star or on other field stars, avoid these difficulties of contrast, and so have become successful and pop ...
... years1 away, the planet appears very close to its star and its faint light is diluted in the glare of its star. Indirect methods designed to detect an exoplanet through its influence on its parent star or on other field stars, avoid these difficulties of contrast, and so have become successful and pop ...
Planet formation in the habitable zone of alpha Centauri B
... The results of the previous section show that, as was the case for α Cen A, the region allowing km-sized planetesimal accretion is much more limited than the one allowing the final stages of planet formation (starting from large embryos): the accretionfriendly zone only extends up to ∼ 0.5 AU for ou ...
... The results of the previous section show that, as was the case for α Cen A, the region allowing km-sized planetesimal accretion is much more limited than the one allowing the final stages of planet formation (starting from large embryos): the accretionfriendly zone only extends up to ∼ 0.5 AU for ou ...
Migration of giant planets in planetesimal discs
... 1995). This standard model predicts nearly circular planetary orbits, and giant planets with orbital distances $1 au from the central star, at which distance the temperature in the protostellar nebula is low enough for icy materials to condense (Boss 1995, 1996; Wuchterl 1993, 1996). Standard disc m ...
... 1995). This standard model predicts nearly circular planetary orbits, and giant planets with orbital distances $1 au from the central star, at which distance the temperature in the protostellar nebula is low enough for icy materials to condense (Boss 1995, 1996; Wuchterl 1993, 1996). Standard disc m ...
GMRT search for 150 MHz radio emission from the transiting
... corrections using 3C48, gain and phase variations of individual antennas were quantified and used for calibrating the flux density, bandpass, gain, and phase for the target field data. For 3C48 we took a flux density of 64.4 Jy at 150 MHz (Perley & Taylor 1999). The calibrated flux densities toward ...
... corrections using 3C48, gain and phase variations of individual antennas were quantified and used for calibrating the flux density, bandpass, gain, and phase for the target field data. For 3C48 we took a flux density of 64.4 Jy at 150 MHz (Perley & Taylor 1999). The calibrated flux densities toward ...
Howard 2013 Observed properties of exoplanets
... few degrees (24). This high degree of follows the same trend as the mass discoplanarity is consistent with planets formtribution, with small planets being more common (16, 17, 18). However, the Kepler Fig. 1. Schematic illustration of a planetary orbit and the var- ing in a disk without substantial ...
... few degrees (24). This high degree of follows the same trend as the mass discoplanarity is consistent with planets formtribution, with small planets being more common (16, 17, 18). However, the Kepler Fig. 1. Schematic illustration of a planetary orbit and the var- ing in a disk without substantial ...
Planetary system formation in thermally evolving viscous
... at least to Cameron [10] and has been the subject of ongoing study since that time [11]. It is now generally agreed that fragmentation is most likely to occur in the low-temperature outer regions of protoplanetary discs where the cooling time is short [12]. Recent discovery of massive gas giant plan ...
... at least to Cameron [10] and has been the subject of ongoing study since that time [11]. It is now generally agreed that fragmentation is most likely to occur in the low-temperature outer regions of protoplanetary discs where the cooling time is short [12]. Recent discovery of massive gas giant plan ...
DIPLOMA THESIS Spectroscopic study of the star 70 Virginis and its
... Marie Hrudková, and programs KOREL and FOTEL, developed by RNDr. Petr Hadrava, DSc. Further, I gratefully acknowledge usage of radial velocities calculated by Dr. D. Naef & al. I am grateful to doc. RNDr. Martin Šolc, CSc. for explanation of the historical background of gravitational microlensing ...
... Marie Hrudková, and programs KOREL and FOTEL, developed by RNDr. Petr Hadrava, DSc. Further, I gratefully acknowledge usage of radial velocities calculated by Dr. D. Naef & al. I am grateful to doc. RNDr. Martin Šolc, CSc. for explanation of the historical background of gravitational microlensing ...
A Bayesian method for the detection of planetary transits
... Another method based on the differential limbdarkening in the red and the blue has been suggested to discriminate between a transit and possible artefacts (Rosenblatt et al. 1971; Borucki & Summers 1984). In fact, this is not an actual detection method but rather a discriminative test. Moreover it n ...
... Another method based on the differential limbdarkening in the red and the blue has been suggested to discriminate between a transit and possible artefacts (Rosenblatt et al. 1971; Borucki & Summers 1984). In fact, this is not an actual detection method but rather a discriminative test. Moreover it n ...
a transiting planet of a sun-like star
... with a fainter, eclipsing binary nearby, which can mimic a transiting planet (Charbonneau et al. 2004). On the basis of the E.T. light curves of 2005, we acquired spectra of XO-1 as described in x 2.3. After the first few spectra showed that XO-1b has substellar mass, we obtained additional photomet ...
... with a fainter, eclipsing binary nearby, which can mimic a transiting planet (Charbonneau et al. 2004). On the basis of the E.T. light curves of 2005, we acquired spectra of XO-1 as described in x 2.3. After the first few spectra showed that XO-1b has substellar mass, we obtained additional photomet ...
Eris is Pluto`s Twin This diagram shows the path of a faint star during
... dwarf planets can help astrobiologists understand the different types of celestial bodies that can exist in orbit around stars. This information is useful in determining how and where to search for habitable worlds around distant stars. While earlier observations using other methods suggested that E ...
... dwarf planets can help astrobiologists understand the different types of celestial bodies that can exist in orbit around stars. This information is useful in determining how and where to search for habitable worlds around distant stars. While earlier observations using other methods suggested that E ...
Potential for Life on the Terrestrial Planets
... Earth-size exoplanets within the habitable zones of their host stars. This important task has been taken over by NASA’s Kepler satellite which is in space since March 2009 (e.g., Borucki et al., 2011). The current limiting precision for the transit method is given by Kepler with ~ 20 ppm. The Earth- ...
... Earth-size exoplanets within the habitable zones of their host stars. This important task has been taken over by NASA’s Kepler satellite which is in space since March 2009 (e.g., Borucki et al., 2011). The current limiting precision for the transit method is given by Kepler with ~ 20 ppm. The Earth- ...
Terrestrial Planets
... the light emanating from a star passes very close to another star on its way to an observer on Earth, the gravity of the intermediary star will slightly bend the light rays from the source star, causing the two stars to appear farther apart than they normally would. This effect was used by Sir Arthu ...
... the light emanating from a star passes very close to another star on its way to an observer on Earth, the gravity of the intermediary star will slightly bend the light rays from the source star, causing the two stars to appear farther apart than they normally would. This effect was used by Sir Arthu ...
Script
... The transit method also makes it possible to study the atmosphere of the transiting planet. When the planet transits the star, light from the star passes through the upper atmosphere of the planet. By studying the high-resolution stellar spectrum carefully, one can detect elements present in the pla ...
... The transit method also makes it possible to study the atmosphere of the transiting planet. When the planet transits the star, light from the star passes through the upper atmosphere of the planet. By studying the high-resolution stellar spectrum carefully, one can detect elements present in the pla ...
1. INTRODUCTION
... HK for the six new Keck planet candiThe orbital parameters dates are listed in Table 2. The quantities in parentheses are the formal uncertainties in each orbital parameter, as determined by Monte Carlo simulations. The individual Keck Doppler velocity measurements are listed in Tables 3 through 8. ...
... HK for the six new Keck planet candiThe orbital parameters dates are listed in Table 2. The quantities in parentheses are the formal uncertainties in each orbital parameter, as determined by Monte Carlo simulations. The individual Keck Doppler velocity measurements are listed in Tables 3 through 8. ...
Habitability of super-Earth planets around main
... In Table 1, we also list the stellar effective temperatures, which are a steep monotonic function of the stellar mass. Note that due to the appearance of increased photospheric UV fluxes, relatively high effective temperatures by themselves represent an adverse factor for the general possibility of a ...
... In Table 1, we also list the stellar effective temperatures, which are a steep monotonic function of the stellar mass. Note that due to the appearance of increased photospheric UV fluxes, relatively high effective temperatures by themselves represent an adverse factor for the general possibility of a ...
The extreme physical properties of the CoRoT-7b super
... Rocky planets located in the habitable zone (HZ) of their star are our present best candidates for harbouring extra-terrestrial life (see for instance Cockell et al., 2009). As a result, the search for rocky exoplanets is of special importance. Super-Earth candidates, planets with masses 1 - 10 MEar ...
... Rocky planets located in the habitable zone (HZ) of their star are our present best candidates for harbouring extra-terrestrial life (see for instance Cockell et al., 2009). As a result, the search for rocky exoplanets is of special importance. Super-Earth candidates, planets with masses 1 - 10 MEar ...
2.4 Statistical properties of radial velocity planets
... G, K main-sequence stars the RV velocity surveys find the following numbers: – for about 1 % of the stars a close in (<0.1 AU), hot Jupiter with mP sin i > 0.1MJ is detected, – for about 15 % of the stars a giant planet with mP sin i > 0.1MJ out to a separation of 5 AU is present, – RV-surveys can n ...
... G, K main-sequence stars the RV velocity surveys find the following numbers: – for about 1 % of the stars a close in (<0.1 AU), hot Jupiter with mP sin i > 0.1MJ is detected, – for about 15 % of the stars a giant planet with mP sin i > 0.1MJ out to a separation of 5 AU is present, – RV-surveys can n ...
Lecture 7: Extrasolar Planets 01/08/2013 update: 725 exoplanets
... Einstein's General Theory of Relativity. According to Einstein, when the light emanating from a star passes very close to another star on its way to an observer on Earth, the gravity of the intermediary star will slightly bend the light rays from the source star, causing the two stars to appear fart ...
... Einstein's General Theory of Relativity. According to Einstein, when the light emanating from a star passes very close to another star on its way to an observer on Earth, the gravity of the intermediary star will slightly bend the light rays from the source star, causing the two stars to appear fart ...
Kepler Mission Workshop Presentation
... lava and much too hot for life as we know it • All five of the exoplanets orbit stars hotter and larger than Earth's sun. ...
... lava and much too hot for life as we know it • All five of the exoplanets orbit stars hotter and larger than Earth's sun. ...
latest Edition - ExoPlanet News
... samples of planet and non-planet hosts. Whether these chemical differences are indeed related to the presence of planets is still strongly debated. Aims. We aim to test whether solar-type stars with debris discs show any chemical peculiarity that could be related to the planet formation process. Met ...
... samples of planet and non-planet hosts. Whether these chemical differences are indeed related to the presence of planets is still strongly debated. Aims. We aim to test whether solar-type stars with debris discs show any chemical peculiarity that could be related to the planet formation process. Met ...
Is there life in space? Activity 1: The Vastness of Space
... means that scientists should be looking for planets that fall into the habitable range—not too close to their stars and not too far away from their stars for liquid water to exist. Students may give other answers, such it must be a rocky planet, or that it needs to have an energy source. These are r ...
... means that scientists should be looking for planets that fall into the habitable range—not too close to their stars and not too far away from their stars for liquid water to exist. Students may give other answers, such it must be a rocky planet, or that it needs to have an energy source. These are r ...
RV Metric_new_8
... The computations answer this question, yes or no, for all 419 planets on every day on the host star’s validity list, for two values of i: “face-on” (0.9°) and “edge-on” (89.1°). In the first step, we compute the three-dimensional position of the planet in space relative to the center of mass, from p ...
... The computations answer this question, yes or no, for all 419 planets on every day on the host star’s validity list, for two values of i: “face-on” (0.9°) and “edge-on” (89.1°). In the first step, we compute the three-dimensional position of the planet in space relative to the center of mass, from p ...
Are planetary systems flat?
... Why might we believe that planetary systems are not flat? • rms eccentricities in extrasolar planetary systems are much larger than in the solar system • mutual inclination of υ And c and d • extrasolar planetary systems are different from the solar system • if planet formation were similar to star ...
... Why might we believe that planetary systems are not flat? • rms eccentricities in extrasolar planetary systems are much larger than in the solar system • mutual inclination of υ And c and d • extrasolar planetary systems are different from the solar system • if planet formation were similar to star ...
Terrestrial planet formation in exoplanetary systems with a giant
... that the 47 Uma system could harbor a terrestrial planet in an orbit that remains confined to the habitable zone. However, these simulations focus on the orbital stability problem, and do not investigate the possibility that such terrestrial planets can actually f orm in these systems. The process o ...
... that the 47 Uma system could harbor a terrestrial planet in an orbit that remains confined to the habitable zone. However, these simulations focus on the orbital stability problem, and do not investigate the possibility that such terrestrial planets can actually f orm in these systems. The process o ...
Gliese 581
Gliese 581 (/ˈɡliːzə/) is a star of spectral type M3V (a red dwarf) about 20 light years away from Earth in the constellation Libra. Its estimated mass is about a third of that of the Sun, and it is the 89th closest known star to the Sun. Observations suggest that the star has a planetary system consisting of three known planets, designated Gliese 581 b, c, and e and a possibly confirmed planet, d, in order of discovery. Additional outer planets, which received the designations Gliese 581 f, and g have been proposed, but the evidence that led to the discovery claims has been shown to be the result of stellar activity mimicking the radial velocity variations due to orbiting planets.Gliese 581 has been the subject of a ""huge amount of attention"" in the quest to discover the first habitable extrasolar planet; first for c, and then d and g. Gliese 581 c, the first low-mass extrasolar planet found near a habitable zone, was discovered in April 2007. It has since been shown that under known terrestrial planet climate models, Gliese 581 c is likely to have a runaway greenhouse effect, and hence is probably too hot to be habitable, analogous to Venus. The proposed planets Gliese 581 d and Gliese 581 g also received attention as being located within the habitable zone, but their existence has subsequently been put into doubt by some authors.On 27 November 2012, the European Space Agency announced a debris disk, with at least ten times as many comets as the Solar System. This put constraints on possible planets beyond 0.75 AU.