Planet formation in the habitable zone of alpha Centauri B
... τdiss = 105 years. The dissipation is started at 104 years, the end of our nominal run, when all orbits have reached their size-dependent alignment in the HZ. Fig.3 shows the dynamical state of the system after 2τdiss = 2x105 years and clearly illustrates the efficient re-phasing of all orbits, whic ...
... τdiss = 105 years. The dissipation is started at 104 years, the end of our nominal run, when all orbits have reached their size-dependent alignment in the HZ. Fig.3 shows the dynamical state of the system after 2τdiss = 2x105 years and clearly illustrates the efficient re-phasing of all orbits, whic ...
student instruction and answer sheet
... orbiting planet. 90% of the stars in our galaxy are too cool to have a sizable habitable zone. This eliminates stars with spectral type K5 and cooler. Of the remaining 10%, nearly a quarter of those have lifetimes too short for life to develop. This eliminates stars warmer with spectral type F8 and ...
... orbiting planet. 90% of the stars in our galaxy are too cool to have a sizable habitable zone. This eliminates stars with spectral type K5 and cooler. Of the remaining 10%, nearly a quarter of those have lifetimes too short for life to develop. This eliminates stars warmer with spectral type F8 and ...
Asynchronous rotation of Earth-mass planets in the habitable zone
... a permanent cold, night side may not be as severe as usually thought. On the other hand, the habitable zone has been recently shown to be more extended for synchronous planets (12). For these objects, if the atmosphere is thick enough, the non-synchronous rotation that will ensue will thus come to l ...
... a permanent cold, night side may not be as severe as usually thought. On the other hand, the habitable zone has been recently shown to be more extended for synchronous planets (12). For these objects, if the atmosphere is thick enough, the non-synchronous rotation that will ensue will thus come to l ...
Planet formation Abstract Megan K Pickett and Andrew J Lim
... images of the disks themselves, at least in principle. It is true that a few face-on protostellar disks exhibit wide-scale asymmetry (figure 3), though their nature and the origin of the nonaxisymmetry is not well determined; it is not clear, for example, whether or not the structure is due to gravi ...
... images of the disks themselves, at least in principle. It is true that a few face-on protostellar disks exhibit wide-scale asymmetry (figure 3), though their nature and the origin of the nonaxisymmetry is not well determined; it is not clear, for example, whether or not the structure is due to gravi ...
Procedurally Generating an Artificial Galaxy
... Imagine the seeds between 0 and 9. They will all output 0. Furthermore, if we run a sequence of seeds through the algorithm, subsequent outputs will be higher with intermittent drops. To get rid of this pattern you need to run the output numbers through the algorithm a few more times. The problem is ...
... Imagine the seeds between 0 and 9. They will all output 0. Furthermore, if we run a sequence of seeds through the algorithm, subsequent outputs will be higher with intermittent drops. To get rid of this pattern you need to run the output numbers through the algorithm a few more times. The problem is ...
The extreme physical properties of the CoRoT-7b super
... giant planet just exterior to a strong mean motion resonance with CoRoT-7b, e.g. 2:1 or 3:2 (Zhou et al, 2005; Fogg & Nelson, 2005; Raymond et al, 2006; Mandell et al., 2007), which is clearly not observed in the HARPS radial velocity data (Queloz et al., 2009). - Scenario (1), given the small amoun ...
... giant planet just exterior to a strong mean motion resonance with CoRoT-7b, e.g. 2:1 or 3:2 (Zhou et al, 2005; Fogg & Nelson, 2005; Raymond et al, 2006; Mandell et al., 2007), which is clearly not observed in the HARPS radial velocity data (Queloz et al., 2009). - Scenario (1), given the small amoun ...
L8 Condensation
... in the solar nebula we must have a suitable model of the solar nebula. In this simple example, let us assume that we have a constant total pressure (the increase of the total pressure due to vaporized Fe is neglected). In a good approximation this total pressure is equal to the hydrogen and helium p ...
... in the solar nebula we must have a suitable model of the solar nebula. In this simple example, let us assume that we have a constant total pressure (the increase of the total pressure due to vaporized Fe is neglected). In a good approximation this total pressure is equal to the hydrogen and helium p ...
pierrehumbert_lecture_1
... heavy molecules into lighter components that escape more easily. • Low mass stars can take a half billion years to enter the main sequence, and UV/X-ray luminosity is further elevated throughout this time. • But as M stars age on the main sequence, they can quiet down If planets can regenerate an at ...
... heavy molecules into lighter components that escape more easily. • Low mass stars can take a half billion years to enter the main sequence, and UV/X-ray luminosity is further elevated throughout this time. • But as M stars age on the main sequence, they can quiet down If planets can regenerate an at ...
UK Exoplanet community meeting 2017
... perspective of exo-planetary systems, whilst at the same time deepening our knowledge of Earth’s formation. Profound questions still remain as to the origin of Earth’s atmosphere, continents, and habitable climate, questions which are ultimately stymied by having only one natural laboratory in which ...
... perspective of exo-planetary systems, whilst at the same time deepening our knowledge of Earth’s formation. Profound questions still remain as to the origin of Earth’s atmosphere, continents, and habitable climate, questions which are ultimately stymied by having only one natural laboratory in which ...