PLANETS
... • Maximum a ~ 3.5 AU (ie orbital period ~ 7 years) • Minimum mass ~ 0.5 Jupiter masses at 1 AU, scaling with square root of semi-major axis • No strong selection bias in favour / against detecting planets with different eccentricities Of the first 100 stars found to harbor planets, more than 30 star ...
... • Maximum a ~ 3.5 AU (ie orbital period ~ 7 years) • Minimum mass ~ 0.5 Jupiter masses at 1 AU, scaling with square root of semi-major axis • No strong selection bias in favour / against detecting planets with different eccentricities Of the first 100 stars found to harbor planets, more than 30 star ...
PLANETS
... • Maximum a ~ 3.5 AU (ie orbital period ~ 7 years) • Minimum mass ~ 0.5 Jupiter masses at 1 AU, scaling with square root of semi-major axis • No strong selection bias in favour / against detecting planets with different eccentricities Of the first 100 stars found to harbour planets, more than 30 sta ...
... • Maximum a ~ 3.5 AU (ie orbital period ~ 7 years) • Minimum mass ~ 0.5 Jupiter masses at 1 AU, scaling with square root of semi-major axis • No strong selection bias in favour / against detecting planets with different eccentricities Of the first 100 stars found to harbour planets, more than 30 sta ...
10. Exoplanets
... • Observations of extrasolar planets have shown that the nebular theory was incomplete. • Effects like planetary migration and gravitational encounters might be more important than previously thought. © 2010 Pearson Education, Inc. ...
... • Observations of extrasolar planets have shown that the nebular theory was incomplete. • Effects like planetary migration and gravitational encounters might be more important than previously thought. © 2010 Pearson Education, Inc. ...
4.1 Detectability of extrasolar planets
... samples and hence both moderate limiting magnitudes and integration times of at most a few hours per target for initial discovery. Science requires statistics – an ExAO system that could detect Earthlike planets but requires such bright stars that it can only observe ten targets may find a single ex ...
... samples and hence both moderate limiting magnitudes and integration times of at most a few hours per target for initial discovery. Science requires statistics – an ExAO system that could detect Earthlike planets but requires such bright stars that it can only observe ten targets may find a single ex ...
Moro_Martin`s Talk - CIERA
... Cold KB-like disks are more common than AB-like disks. Individual collisional events may dominate disk properties. Inner gaps appear to be common in cold KB-like disks ...
... Cold KB-like disks are more common than AB-like disks. Individual collisional events may dominate disk properties. Inner gaps appear to be common in cold KB-like disks ...
Chapter 15 The Formation of Planetary Systems
... planet will then eclipse the star, and if the planet is large enough, a (very small!) decrease in luminosity may be observed as a function of time. This is called a transit. Notice a transit requires a planetary orbit almost perfectly in the line of sight of an observer on Earth. So transits will be ...
... planet will then eclipse the star, and if the planet is large enough, a (very small!) decrease in luminosity may be observed as a function of time. This is called a transit. Notice a transit requires a planetary orbit almost perfectly in the line of sight of an observer on Earth. So transits will be ...
Chapter 15 The Formation of Planetary Systems
... planet will then eclipse the star, and if the planet is large enough, a (very small!) decrease in luminosity may be observed as a function of time. This is called a transit. Notice a transit requires a planetary orbit almost perfectly in the line of sight of an observer on Earth. So transits will be ...
... planet will then eclipse the star, and if the planet is large enough, a (very small!) decrease in luminosity may be observed as a function of time. This is called a transit. Notice a transit requires a planetary orbit almost perfectly in the line of sight of an observer on Earth. So transits will be ...
The Discovery of Planets beyond the Solar System
... With a pair of exceptions, all discovered planets move very close to their stars. . This is due to the Doppler effect used in most discoveries: the star motion is larger when the planet going around is closer ...
... With a pair of exceptions, all discovered planets move very close to their stars. . This is due to the Doppler effect used in most discoveries: the star motion is larger when the planet going around is closer ...
Potential for Life on the Terrestrial Planets
... by hydrogen envelopes or dense hydrogen-rich volatiles containing a few percent of their masses (e.g., Lissauer et al., 2011; Ikoma and Hori, 2012; Lammer et al., 2013). The existance of such envelopes indicates that these planets did not get rid of their nebulabased or outgassed protoatmospheres (K ...
... by hydrogen envelopes or dense hydrogen-rich volatiles containing a few percent of their masses (e.g., Lissauer et al., 2011; Ikoma and Hori, 2012; Lammer et al., 2013). The existance of such envelopes indicates that these planets did not get rid of their nebulabased or outgassed protoatmospheres (K ...
transit observations of new planets
... this was done for planets within our solar system. Now this search has expanded to include a much greater area our galaxy. One way in which the search is conducted is via the “Transit” method. A transit occurs when an object passes in front of a star. When this happens, some of the light coming from ...
... this was done for planets within our solar system. Now this search has expanded to include a much greater area our galaxy. One way in which the search is conducted is via the “Transit” method. A transit occurs when an object passes in front of a star. When this happens, some of the light coming from ...
Activity I: Plotting a Light Curve due to a Transit
... this dip in intensity repeated every 3.52 days. From the drop in intensity and the length of the period we can tell a number of things about the planet. The drop in intensity can lead us to tell the size of the planet and thus, if it is large enough to hold an atmosphere. The period of the planet wi ...
... this dip in intensity repeated every 3.52 days. From the drop in intensity and the length of the period we can tell a number of things about the planet. The drop in intensity can lead us to tell the size of the planet and thus, if it is large enough to hold an atmosphere. The period of the planet wi ...
Chapter 13 Power Point Lecture
... • We cannot measure an exact mass for a planet without knowing the tilt of its orbit, because Doppler shift tells us only the velocity toward or away from us. • Doppler data give us lower limits on masses. © 2014 Pearson Education, Inc. ...
... • We cannot measure an exact mass for a planet without knowing the tilt of its orbit, because Doppler shift tells us only the velocity toward or away from us. • Doppler data give us lower limits on masses. © 2014 Pearson Education, Inc. ...
A Brief History of the Solar System
... it becomes so hot that two hydrogen atoms are fused releasing enormous amount of nuclear energy. If the process of nuclear burning at the core of the region continues, then the protostar becomes a main-sequence star. However, if the mass of the central region is less than the critical mass for nucle ...
... it becomes so hot that two hydrogen atoms are fused releasing enormous amount of nuclear energy. If the process of nuclear burning at the core of the region continues, then the protostar becomes a main-sequence star. However, if the mass of the central region is less than the critical mass for nucle ...
Chap1-Introduction - Groupe d`astrophysique de UdeM
... • Low-mass planets appear to be very common. ...
... • Low-mass planets appear to be very common. ...
Introduction
... measurements of the host star. In this Section, we briefly review this and other techniques used to detect exoplanets, paying special attention to their major findings and the current status. After that (Section 1.2), we will concentrate on the transit method, providing the planetary parameters that ...
... measurements of the host star. In this Section, we briefly review this and other techniques used to detect exoplanets, paying special attention to their major findings and the current status. After that (Section 1.2), we will concentrate on the transit method, providing the planetary parameters that ...
A rocky planet transiting a nearby low-mass star
... of eight 40-cm robotic telescopes located at the Cerro Tololo Inter-American Observatory (CTIO) in Chile, and observes a sample of M-dwarf stars that are within 33 parsecs of Earth and smaller than 0.35 solar radii. Since early 2014, the telescopes have gathered data almost every night that weather ...
... of eight 40-cm robotic telescopes located at the Cerro Tololo Inter-American Observatory (CTIO) in Chile, and observes a sample of M-dwarf stars that are within 33 parsecs of Earth and smaller than 0.35 solar radii. Since early 2014, the telescopes have gathered data almost every night that weather ...
Debris Belts around Vega - Astronomical Society of the Pacific
... “transit” method, since they wouldn’t pass in front of the star from our perspective. • We can’t detect planets by the “Doppler” method because stars like Vega rotate very fast and have very few narrow lines in their spectra Credit: NASA/JPL-Caltech for detection of the tiny shifts in line position ...
... “transit” method, since they wouldn’t pass in front of the star from our perspective. • We can’t detect planets by the “Doppler” method because stars like Vega rotate very fast and have very few narrow lines in their spectra Credit: NASA/JPL-Caltech for detection of the tiny shifts in line position ...
PDF format
... – Transit missions will be capable of finding Earth-like planets that cross in front of their stars. – Astrometric missions will be capable of measuring the "wobble" of a star caused by an orbiting Earth-like planet. – Missions for direct detection of an Earth-like planet will need to use special ...
... – Transit missions will be capable of finding Earth-like planets that cross in front of their stars. – Astrometric missions will be capable of measuring the "wobble" of a star caused by an orbiting Earth-like planet. – Missions for direct detection of an Earth-like planet will need to use special ...
DATA FROM CATALOGUES OF SOLAR SYSTEM OBJECTS IN
... I used data for list of minor planets from official Minor Planet Center (MPC) available at www.minorplanetcenter.net. Web pages of MPC do not have any graphical output of these data. They are available just in the text form – as a file with size of tens of MB. As mentioned before it is not suitable ...
... I used data for list of minor planets from official Minor Planet Center (MPC) available at www.minorplanetcenter.net. Web pages of MPC do not have any graphical output of these data. They are available just in the text form – as a file with size of tens of MB. As mentioned before it is not suitable ...
pluto: a human comedy
... place from which they were observed. These facts could be organised into a workable model, if one imagined a round Earth which rotated with a period of one day, about an axis which pointed in a direction very close to the position of the Polaris. This model is, of course, consistent with the notion ...
... place from which they were observed. These facts could be organised into a workable model, if one imagined a round Earth which rotated with a period of one day, about an axis which pointed in a direction very close to the position of the Polaris. This model is, of course, consistent with the notion ...
New planets in the solar system — Uranus, Ceres and so on
... are dealt with in detail in many other papers and books. The emergence of the socalled Bode’s law played a role in connection with the search for new planets. However, it was not decisive for the questions discussed here. Also the already systematic search for an unknown planet beyond Uranus which l ...
... are dealt with in detail in many other papers and books. The emergence of the socalled Bode’s law played a role in connection with the search for new planets. However, it was not decisive for the questions discussed here. Also the already systematic search for an unknown planet beyond Uranus which l ...
Terrestrial Planets
... However, when bodies in this zone collide, they initiate cascades of further collisions among the debris and between it and other members of the system, eventually grinding a significant amount of material into dust grains distributed in a so-called debris disk. Because the grains have larger surfac ...
... However, when bodies in this zone collide, they initiate cascades of further collisions among the debris and between it and other members of the system, eventually grinding a significant amount of material into dust grains distributed in a so-called debris disk. Because the grains have larger surfac ...
6 March 2013 Exoplanets and Where to Find Them Professor
... parts of the disc are inclined at about 5° relative to the outer regions. When first discovered, the disturbances (particularly the clear dust-free gap) were attributed to the presence of one or more exoplanets in the system, and in 2008 infrared images finally detected a point source in this clear ...
... parts of the disc are inclined at about 5° relative to the outer regions. When first discovered, the disturbances (particularly the clear dust-free gap) were attributed to the presence of one or more exoplanets in the system, and in 2008 infrared images finally detected a point source in this clear ...
Exoplanets
... of the extreme contrast between the light emitted by the parent star and by the companion planet. To expose the planet, the starlight must be dimmed or masked in some way so as to enable observers to see into the shadow. One method is to use infrared radiation, rather than visible light. The visible ...
... of the extreme contrast between the light emitted by the parent star and by the companion planet. To expose the planet, the starlight must be dimmed or masked in some way so as to enable observers to see into the shadow. One method is to use infrared radiation, rather than visible light. The visible ...
An optical/UV space coronagraph concept for the terrestrial planet finder
... limited and there will always be a residual halo of scattered starlight near the planet. A common parameter for measuring this error is Q, the ratio of planet light to the residual background (Brown & Burrows, 1990). It is conceptually useful to divide the various error sources into two categories—s ...
... limited and there will always be a residual halo of scattered starlight near the planet. A common parameter for measuring this error is Q, the ratio of planet light to the residual background (Brown & Burrows, 1990). It is conceptually useful to divide the various error sources into two categories—s ...
Kepler (spacecraft)
Kepler is a space observatory launched by NASA to discover Earth-like planets orbiting other stars. The spacecraft, named after the German Renaissance astronomer Johannes Kepler, was launched on March 7, 2009.Designed to survey a portion of our region of the Milky Way to discover dozens of Earth-size extrasolar planets in or near the habitable zone and estimate how many of the billions of stars in the Milky Way have such planets, Kepler's sole instrument is a photometer that continually monitors the brightness of over 145,000 main sequence stars in a fixed field of view. This data is transmitted to Earth, then analyzed to detect periodic dimming caused by extrasolar planets that cross in front of their host star.Kepler is part of NASA's Discovery Program of relatively low-cost, focused primary science missions. The telescope's construction and initial operation were managed by NASA's Jet Propulsion Laboratory, with Ball Aerospace responsible for developing the Kepler flight system. The Ames Research Center is responsible for the ground system development, mission operations since December 2009, and scientific data analysis. The initial planned lifetime was 3.5 years, but greater-than-expected noise in the data, from both the stars and the spacecraft, meant additional time was needed to fulfill all mission goals. Initially, in 2012, the mission was expected to last until 2016, but this would only have been possible if all remaining reaction wheels used for pointing the spacecraft remained reliable. On May 11, 2013, a second of four reaction wheels failed, disabling the collection of science data and threatening the continuation of the mission.On August 15, 2013, NASA announced that they had given up trying to fix the two failed reaction wheels. This meant the current mission needed to be modified, but it did not necessarily mean the end of planet-hunting. NASA had asked the space science community to propose alternative mission plans ""potentially including an exoplanet search, using the remaining two good reaction wheels and thrusters"". On November 18, 2013, the K2 ""Second Light"" proposal was reported. This would include utilizing the disabled Kepler in a way that could detect habitable planets around smaller, dimmer red dwarfs. On May 16, 2014, NASA announced the approval of the K2 extension.As of January 2015, Kepler and its follow-up observations had found 1,013 confirmed exoplanets in about 440 stellar systems, along with a further 3,199 unconfirmed planet candidates. Four planets have been confirmed through Kepler 's K2 mission. In November 2013, astronomers reported, based on Kepler space mission data, that there could be as many as 40 billion Earth-sized planets orbiting in the habitable zones of Sun-like stars and red dwarfs within the Milky Way. It is estimated that 11 billion of these planets may be orbiting Sun-like stars. The nearest such planet may be 3.7 parsecs (12 ly) away, according to the scientists.On January 6, 2015, NASA announced the 1000th confirmed exoplanet discovered by the Kepler Space Telescope. Four of the newly confirmed exoplanets were found to orbit within habitable zones of their related stars: three of the four, Kepler-438b, Kepler-442b and Kepler-452b, are near-Earth-size and likely rocky; the fourth, Kepler-440b, is a super-Earth.