Chap1-Introduction - Groupe d`astrophysique de UdeM
... The fraction of low-mass stars with an Earth/super-Earths in the habitable zone (HZ) is significant (at least 10, perhaps as much as 100%). A handful of HZ Earths/super-Earths have been identified. ...
... The fraction of low-mass stars with an Earth/super-Earths in the habitable zone (HZ) is significant (at least 10, perhaps as much as 100%). A handful of HZ Earths/super-Earths have been identified. ...
Figueira, Pont, Mordasini, Alibert, Georgy, Benz
... process in the inner disk, creating a population of which the hot Neptune is representative. Key words. planetary systems - planetary systems: formation - stars: individual: GJ 436 ...
... process in the inner disk, creating a population of which the hot Neptune is representative. Key words. planetary systems - planetary systems: formation - stars: individual: GJ 436 ...
an Educator`s GuidE
... These exoplanets are very far away, so how do we actually “see” them? Exoplanets are nearly impossible to photograph in the traditional sense, so we have to find them by observing the effects they have on their parent stars. These effects, driven by gravity and line-of-sight, are visible to us as ei ...
... These exoplanets are very far away, so how do we actually “see” them? Exoplanets are nearly impossible to photograph in the traditional sense, so we have to find them by observing the effects they have on their parent stars. These effects, driven by gravity and line-of-sight, are visible to us as ei ...
an Educator`s GuidE
... These exoplanets are very far away, so how do we actually “see” them? Exoplanets are nearly impossible to photograph in the traditional sense, so we have to find them by observing the effects they have on their parent stars. These effects, driven by gravity and line-of-sight, are visible to us as ei ...
... These exoplanets are very far away, so how do we actually “see” them? Exoplanets are nearly impossible to photograph in the traditional sense, so we have to find them by observing the effects they have on their parent stars. These effects, driven by gravity and line-of-sight, are visible to us as ei ...
an Educator`s GuidE - Museum of Science, Boston
... These exoplanets are very far away, so how do we actually “see” them? Exoplanets are nearly impossible to photograph in the traditional sense, so we have to find them by observing the effects they have on their parent stars. These effects, driven by gravity and line-of-sight, are visible to us as ei ...
... These exoplanets are very far away, so how do we actually “see” them? Exoplanets are nearly impossible to photograph in the traditional sense, so we have to find them by observing the effects they have on their parent stars. These effects, driven by gravity and line-of-sight, are visible to us as ei ...
The Search for Planet X Transcript
... Charon. Charon was the ferryman who carried the dead across the river Styx and had close ties to Pluto so was an ideal name. Its first 4 letters were also the same as those of Christy's wife Charlene! If the period and semi-major axis of a satellite are known, it is possible to calculate the mass of ...
... Charon. Charon was the ferryman who carried the dead across the river Styx and had close ties to Pluto so was an ideal name. Its first 4 letters were also the same as those of Christy's wife Charlene! If the period and semi-major axis of a satellite are known, it is possible to calculate the mass of ...
T
... The long-term precision of the instrument cannot be checked easily because it requires a long time base on one hand, and the knowledge of stable stellar sources on the other hand. Especially the latter point represents a new challenge since the intrinsic stability of the stars has never been studied ...
... The long-term precision of the instrument cannot be checked easily because it requires a long time base on one hand, and the knowledge of stable stellar sources on the other hand. Especially the latter point represents a new challenge since the intrinsic stability of the stars has never been studied ...
Undiscovered Worlds educators guide
... These exoplanets are very far away, so how do we actually “see” them? Exoplanets are nearly impossible to photograph in the traditional sense, so we have to find them by observing the effects they have on their parent stars. These effects, driven by gravity and line-of-sight, are visible to us as ei ...
... These exoplanets are very far away, so how do we actually “see” them? Exoplanets are nearly impossible to photograph in the traditional sense, so we have to find them by observing the effects they have on their parent stars. These effects, driven by gravity and line-of-sight, are visible to us as ei ...
The Search for Exoplanets - Worcester Polytechnic Institute
... During the 8th and 9th Centuries, the Arab world benefitted greatly from an influx of ancient texts from many sources across the known world. Not only did they receive the previously-mentioned Indian and Persian texts from the demise of the Sassanids, but following a ceasefire with the Byzantine Emp ...
... During the 8th and 9th Centuries, the Arab world benefitted greatly from an influx of ancient texts from many sources across the known world. Not only did they receive the previously-mentioned Indian and Persian texts from the demise of the Sassanids, but following a ceasefire with the Byzantine Emp ...
Transit detecion on eclipsing binary systems
... EB Transit detection algorithm (TDA) development Jenkins,Doyle & Cullers 1996: propose a matching filter TDA.The detection statistics C is obtained from a scalar multiplication of the vectors representing model-lc and observed data. Jenkins et al. present this TDA in the context of the transit dete ...
... EB Transit detection algorithm (TDA) development Jenkins,Doyle & Cullers 1996: propose a matching filter TDA.The detection statistics C is obtained from a scalar multiplication of the vectors representing model-lc and observed data. Jenkins et al. present this TDA in the context of the transit dete ...
13_Testbank - Lick Observatory
... so the density is M/V = 0.27 grams per cubic centimeter. The average density of Jupiter is 1.33 grams per cubic centimeter, so HD 209458b is five times less dense. This is due to it being "puffed up" from the high temperatures in such a close orbit around its host star. 6) The star Rho Cancri B has ...
... so the density is M/V = 0.27 grams per cubic centimeter. The average density of Jupiter is 1.33 grams per cubic centimeter, so HD 209458b is five times less dense. This is due to it being "puffed up" from the high temperatures in such a close orbit around its host star. 6) The star Rho Cancri B has ...
Chap4-Timing
... All planets within the final extent of the red giant envelope will be engulfed and migrate inwards. Planets further out will have greater chance of survival, migrating outwards as mass is lost from central star. In mass is loss instantaneously, planet could escape the system. Planetary orbit ...
... All planets within the final extent of the red giant envelope will be engulfed and migrate inwards. Planets further out will have greater chance of survival, migrating outwards as mass is lost from central star. In mass is loss instantaneously, planet could escape the system. Planetary orbit ...
Other Planetary Systems The New Science of Distant Worlds 13.1
... so the density is M/V = 0.27 grams per cubic centimeter. The average density of Jupiter is 1.33 grams per cubic centimeter, so HD 209458b is five times less dense. This is due to it being "puffed up" from the high temperatures in such a close orbit around its host star. 6) The star Rho Cancri B has ...
... so the density is M/V = 0.27 grams per cubic centimeter. The average density of Jupiter is 1.33 grams per cubic centimeter, so HD 209458b is five times less dense. This is due to it being "puffed up" from the high temperatures in such a close orbit around its host star. 6) The star Rho Cancri B has ...
Planet Formation
... system of vortices present around the Sun. Then, later, in 1734, Emanuel Swedenborg was the one to propose the nebular hypothesis, which would be the basis for modern thoughts on planet formation. It states that the planets formed from a cloud of dust present around the Sun. In 1755 Immanuel Kant fu ...
... system of vortices present around the Sun. Then, later, in 1734, Emanuel Swedenborg was the one to propose the nebular hypothesis, which would be the basis for modern thoughts on planet formation. It states that the planets formed from a cloud of dust present around the Sun. In 1755 Immanuel Kant fu ...
Age aspects of habitability - Cambridge University Press
... Abstract: A ‘habitable zone’ of a star is defined as a range of orbits within which a rocky planet can support liquid water on its surface. The most intriguing question driving the search for habitable planets is whether they host life. But is the age of the planet important for its habitability? If ...
... Abstract: A ‘habitable zone’ of a star is defined as a range of orbits within which a rocky planet can support liquid water on its surface. The most intriguing question driving the search for habitable planets is whether they host life. But is the age of the planet important for its habitability? If ...
Prospects for detection of protoplanets
... probe the colder dust and thus the global dust content in disks: • Beckwith et al. (1990): no evidence of temporal evolution in the mass of cold, small (<1mm) dust particles between ages of 0.1 and 10Myr • By an age of 300 Myr the dust masses were found to by decreased by at least 2 orders of magnit ...
... probe the colder dust and thus the global dust content in disks: • Beckwith et al. (1990): no evidence of temporal evolution in the mass of cold, small (<1mm) dust particles between ages of 0.1 and 10Myr • By an age of 300 Myr the dust masses were found to by decreased by at least 2 orders of magnit ...
The Detection and Characterization of Extrasolar Planets
... Given that these are all giant planets, they are unlikely to have conditions suitable for life. However, being able to directly observe and characterize such planets is a step towards being able to do so for less-massive, closer-in planets that may have conditions that make life possible. Additional ...
... Given that these are all giant planets, they are unlikely to have conditions suitable for life. However, being able to directly observe and characterize such planets is a step towards being able to do so for less-massive, closer-in planets that may have conditions that make life possible. Additional ...
On the correlation between stellar chromospheric flux and the
... their planets. Stars with low-gravity planets have on average a lower chromospheric flux. Methods. We propose that this correlation is due to the absorption by circumstellar matter that comes from the evaporation of the planets. Planets with a lower gravity have a greater mass-loss rate which leads ...
... their planets. Stars with low-gravity planets have on average a lower chromospheric flux. Methods. We propose that this correlation is due to the absorption by circumstellar matter that comes from the evaporation of the planets. Planets with a lower gravity have a greater mass-loss rate which leads ...
Habitability and Life Parameters in our Solar System
... million. Afterwards it was introduced the concept of the term “Goldilocks Zone” through exploration of Space Colonization specifically a region around a star whose temperature is just right for water to be present in the liquid phase. Similarly the galactic habitable zones are the regions where life ...
... million. Afterwards it was introduced the concept of the term “Goldilocks Zone” through exploration of Space Colonization specifically a region around a star whose temperature is just right for water to be present in the liquid phase. Similarly the galactic habitable zones are the regions where life ...
Finding habitable earths around white dwarfs with a robotic
... the WDHZ will be the most probable planets to detect. Of course the transit detection probability needs to be folded with planet frequency as a function of a, to obtain the detected planet distribution, and Figure 2 shows that if planets are distribution uniformly in log a down to 2aR , the transiti ...
... the WDHZ will be the most probable planets to detect. Of course the transit detection probability needs to be folded with planet frequency as a function of a, to obtain the detected planet distribution, and Figure 2 shows that if planets are distribution uniformly in log a down to 2aR , the transiti ...
Prospects for Characterizing the Atmosphere of Proxima Centauri b
... exciting discovery of a potentially habitable planet orbiting our nearest neighboring star, Proxima Centauri. The planet has a minimum mass of 1.3 M⊕ and an insolation equal to two thirds that of Earth, suggesting that it could have a rocky surface with temperatures appropriate for the existence of ...
... exciting discovery of a potentially habitable planet orbiting our nearest neighboring star, Proxima Centauri. The planet has a minimum mass of 1.3 M⊕ and an insolation equal to two thirds that of Earth, suggesting that it could have a rocky surface with temperatures appropriate for the existence of ...
Fomalhaut b
... image; cut traces the material surface density of the structure rather than its brightness. ...
... image; cut traces the material surface density of the structure rather than its brightness. ...
Primary and secondary eclipse spectroscopy with JWST: exploring
... or ices, of non-solar composition. This volatile content represents a small fraction of the total planetary mass and is fractionated between the interior (crust, mantle), the surface oceans and/or ice sheets, the atmosphere and outer space through gravitational escape (induced by impacts, exospheric ...
... or ices, of non-solar composition. This volatile content represents a small fraction of the total planetary mass and is fractionated between the interior (crust, mantle), the surface oceans and/or ice sheets, the atmosphere and outer space through gravitational escape (induced by impacts, exospheric ...
Seeing another Earth: Detecting and Characterizing Rocky Planets
... MEare common. In addition to these direct detections, IRAS and Spitzer data show that 20% to 50% of young 1-2 Msunstars are surrounded by dusty disks of debris. This debris is almost certainly material left over from the process of planet formation. Thus, the statistics for the microlensing, radi ...
... MEare common. In addition to these direct detections, IRAS and Spitzer data show that 20% to 50% of young 1-2 Msunstars are surrounded by dusty disks of debris. This debris is almost certainly material left over from the process of planet formation. Thus, the statistics for the microlensing, radi ...
A scenario of planet erosion by coronal radiation*
... The sample of known exoplanets is by no means complete. Several selection effects could be present. (i) With the methods used in exoplanet surveys, it is easier to detect massive planets close to stars. This should bring more massive planets with high FX into our sample, thereby yielding a positive r ...
... The sample of known exoplanets is by no means complete. Several selection effects could be present. (i) With the methods used in exoplanet surveys, it is easier to detect massive planets close to stars. This should bring more massive planets with high FX into our sample, thereby yielding a positive r ...
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.