The Official Magazine of the University Of St Andrews Astronomical Society 1
... Solar Flares and Planetary Migration The vast majority of exoplanets found have been large gas giants, close to their parent star, with orbital periods of only a few days. Our gas giants, however, are orders of magnitude more distant from the sun than typical exoplanets are from their stars. Why is ...
... Solar Flares and Planetary Migration The vast majority of exoplanets found have been large gas giants, close to their parent star, with orbital periods of only a few days. Our gas giants, however, are orders of magnitude more distant from the sun than typical exoplanets are from their stars. Why is ...
The physics of star formation
... processes of star formation, with emphasis on the processes occurring on small scales in star-forming molecular clouds. Previous reviews of the small-scale processes of star formation include those by Hayashi (1966), Larson (1973), Tohline (1982), Shu et al (1987, 1993), Bodenheimer (1992), Hartmann ...
... processes of star formation, with emphasis on the processes occurring on small scales in star-forming molecular clouds. Previous reviews of the small-scale processes of star formation include those by Hayashi (1966), Larson (1973), Tohline (1982), Shu et al (1987, 1993), Bodenheimer (1992), Hartmann ...
Powerpoint slides - Earth & Planetary Sciences
... to presence of nebular gas disk (which then dissipated) – The reason they didn’t just fall into the star is because the disk is absent very close in, probably because it gets cleared away by the star’s magnetic field. An alternative is that tidal torques from the star (just like the Earth-Moon syste ...
... to presence of nebular gas disk (which then dissipated) – The reason they didn’t just fall into the star is because the disk is absent very close in, probably because it gets cleared away by the star’s magnetic field. An alternative is that tidal torques from the star (just like the Earth-Moon syste ...
Full Article - Starry Night Software
... Let’s review the seven planets’ physical characteristics. Many parameters have been calculated, including their sizes, masses, and densities, their average surface temperatures, and the amount of irradiation (sunlight) they receive. We are least certain about the TRAPPIST-1h values because fewer tra ...
... Let’s review the seven planets’ physical characteristics. Many parameters have been calculated, including their sizes, masses, and densities, their average surface temperatures, and the amount of irradiation (sunlight) they receive. We are least certain about the TRAPPIST-1h values because fewer tra ...
Fomalhaut b
... #2 From how bright it is in the optical, and non-detection in the infrared…. less than 3 Jupiter masses. Other sources of optical luminosity are possible: glowing hot gas and/or reflected light from a circumplanetary disk ...
... #2 From how bright it is in the optical, and non-detection in the infrared…. less than 3 Jupiter masses. Other sources of optical luminosity are possible: glowing hot gas and/or reflected light from a circumplanetary disk ...
The Circumstellar Environments of Young Stars at AU Scales
... emission (Millan-Gabet et al., 1999). The measured size was unexpectedly large in the context of then-current disk models of HAeBe objects (e.g., Hillenbrand et al., 1992), which predicted NIR diameter of 0.2 AU based on optically thick, geometrically thin circumstellar disks with a small dust-free ...
... emission (Millan-Gabet et al., 1999). The measured size was unexpectedly large in the context of then-current disk models of HAeBe objects (e.g., Hillenbrand et al., 1992), which predicted NIR diameter of 0.2 AU based on optically thick, geometrically thin circumstellar disks with a small dust-free ...
7.4 Evolution on the Main-Sequence Main-sequence (m
... amount of mass on the m-s. 7.5 Evolution off the Main-Sequence to the Red Giant Branch At the end of central hydrogen fusion, the star has a helium core surrounded by a shell source where H fusion continues. The helium core grows as a result of “ash” from the H-burning shell and contracts under grav ...
... amount of mass on the m-s. 7.5 Evolution off the Main-Sequence to the Red Giant Branch At the end of central hydrogen fusion, the star has a helium core surrounded by a shell source where H fusion continues. The helium core grows as a result of “ash” from the H-burning shell and contracts under grav ...
Study Guide for 3RD Astronomy Exam
... Interpret stellar apparent magnitudes and their relationship to brightness Interpret stellar absolute magnitudes and their relationship to luminosity Solve problems relating to the relative brightness or luminosity of two stars given their m or M values. Determine the hottest and coolest stars from ...
... Interpret stellar apparent magnitudes and their relationship to brightness Interpret stellar absolute magnitudes and their relationship to luminosity Solve problems relating to the relative brightness or luminosity of two stars given their m or M values. Determine the hottest and coolest stars from ...
Stellar Evolution
... • These tiny stars are much smaller than planet Earth -- in fact, they are about the diameter of a large city (~20 km). • One cubic centimeter (like a sugar cube) of a neutron star, would have a mass of about 1011 kg! (hundreds of billions of pounds!) ...
... • These tiny stars are much smaller than planet Earth -- in fact, they are about the diameter of a large city (~20 km). • One cubic centimeter (like a sugar cube) of a neutron star, would have a mass of about 1011 kg! (hundreds of billions of pounds!) ...
The physics of star formation
... with which stars are formed. The structures of galaxies depend on the circumstances in which stars form and the rate at which they form, while the evolution of galaxies depends on the spectrum of masses with which they form, since low-mass stars are faint and evolve slowly while massive ones evolve ...
... with which stars are formed. The structures of galaxies depend on the circumstances in which stars form and the rate at which they form, while the evolution of galaxies depends on the spectrum of masses with which they form, since low-mass stars are faint and evolve slowly while massive ones evolve ...
The physics of star formation - Yale Astronomy
... with which stars are formed. The structures of galaxies depend on the circumstances in which stars form and the rate at which they form, while the evolution of galaxies depends on the spectrum of masses with which they form, since low-mass stars are faint and evolve slowly while massive ones evolve ...
... with which stars are formed. The structures of galaxies depend on the circumstances in which stars form and the rate at which they form, while the evolution of galaxies depends on the spectrum of masses with which they form, since low-mass stars are faint and evolve slowly while massive ones evolve ...
Powerpoint
... How old, and how long do they live? What is their chemical composition? How are they moving? Are they isolated or in clusters? By answering these questions, we not only learn about stars, but about the structure and evolution of galaxies they live in, and the ...
... How old, and how long do they live? What is their chemical composition? How are they moving? Are they isolated or in clusters? By answering these questions, we not only learn about stars, but about the structure and evolution of galaxies they live in, and the ...
thick disk - asteroSTEP
... • a gas-rich merger (Brook et al 2004, 2005). The thick disk stars are born in-situ • accretion (Abadi 2003). The thick disk stars come in from outside • heating of the early thin disk by accretion of a massive satellite • radial migration (stars on more energetic orbits migrate out from the inner g ...
... • a gas-rich merger (Brook et al 2004, 2005). The thick disk stars are born in-situ • accretion (Abadi 2003). The thick disk stars come in from outside • heating of the early thin disk by accretion of a massive satellite • radial migration (stars on more energetic orbits migrate out from the inner g ...
Nebulae - Innovative Teachers BG
... Planetary Nebulae Planetary nebulae in their Photography by Emil Ivanov physical nature are different from nebulae discussed above and being essentially gas-dust clouds. Planetary nebula is an evolution phase of stars with masses 7-8 solar masses and greater. When a star forward in its evolution, l ...
... Planetary Nebulae Planetary nebulae in their Photography by Emil Ivanov physical nature are different from nebulae discussed above and being essentially gas-dust clouds. Planetary nebula is an evolution phase of stars with masses 7-8 solar masses and greater. When a star forward in its evolution, l ...
predictions for the correlation between giant and
... Jupiter, albeit for a much smaller distance, is also predicted within such models and may have left its own signature in the distribution of Hilda asteroids (Franklin et al. 2004). There is no near or medium term prospect for obtaining observations that would permit directly comparable studies in ex ...
... Jupiter, albeit for a much smaller distance, is also predicted within such models and may have left its own signature in the distribution of Hilda asteroids (Franklin et al. 2004). There is no near or medium term prospect for obtaining observations that would permit directly comparable studies in ex ...
Extra-solar planets - Centro de Astrofísica da Universidade do Porto
... or pulsar timing will not be described here. For more details on these two techniques, we point the reader to Beaulieu et al. (2006) and Wolszczan and Frail (1992), and references therein. High angular resolution imaging will also not be deeply discussed, since other chapters in this book approach t ...
... or pulsar timing will not be described here. For more details on these two techniques, we point the reader to Beaulieu et al. (2006) and Wolszczan and Frail (1992), and references therein. High angular resolution imaging will also not be deeply discussed, since other chapters in this book approach t ...
What is a planet? - X-ray and Observational Astronomy Group
... massive, close-in planets • It is not yet sensitive to planets as small as Earth, even close-in • As orbital period increases, the method becomes insensitive to planets less massive than Jupiter • The length of time that the surveys have been active (since 1989) sets the upper orbital period limit – ...
... massive, close-in planets • It is not yet sensitive to planets as small as Earth, even close-in • As orbital period increases, the method becomes insensitive to planets less massive than Jupiter • The length of time that the surveys have been active (since 1989) sets the upper orbital period limit – ...
Gilmore
... Apparently dark-matter dominated ~ 10km/s, 10 < M/L < 100 Metal-poor, all contain very old stars; but ...
... Apparently dark-matter dominated ~ 10km/s, 10 < M/L < 100 Metal-poor, all contain very old stars; but ...
Power Point Presentation
... Disk of gas rotates and fragments around dust nuclei– each fragment spins faster as it collapses (to conserve angular momentum) Accretion and collisions build up the mass of the fragments into planetesimals Planetesimals coalesce to form larger bodies ...
... Disk of gas rotates and fragments around dust nuclei– each fragment spins faster as it collapses (to conserve angular momentum) Accretion and collisions build up the mass of the fragments into planetesimals Planetesimals coalesce to form larger bodies ...