Integrative Studies 410 Our Place in the Universe
... Protostellar Evolution • increasing temperature at core slows contraction – Luminosity about 1000 times that of the sun – Duration ~ 1 million years – Temperature ~ 1 million K at core, 3,000 K at surface • Still too cool for nuclear fusion! ...
... Protostellar Evolution • increasing temperature at core slows contraction – Luminosity about 1000 times that of the sun – Duration ~ 1 million years – Temperature ~ 1 million K at core, 3,000 K at surface • Still too cool for nuclear fusion! ...
Life of a star - bahringcarthnoians
... enough to swallow the inner planets, up to Earth. But don’t panic, because this won’t happen for about 4.5 billion years. ...
... enough to swallow the inner planets, up to Earth. But don’t panic, because this won’t happen for about 4.5 billion years. ...
Lecture (Powerpoint)
... Collapse will usually happen in many places throughout the cloud at the same time This is why stars tend to be clustered Amount of stars depends on size of gas cloud producing stars ...
... Collapse will usually happen in many places throughout the cloud at the same time This is why stars tend to be clustered Amount of stars depends on size of gas cloud producing stars ...
Number of planets - Associazione Astrofili "Crab Nebula"
... in, dragging the lighter elements outward – mostly hydrogen and helium. As the temperature of proto-Sun rose high enough to ignite thermo-nuclear reactions, some bodies inside the disk began to grow by collision and ...
... in, dragging the lighter elements outward – mostly hydrogen and helium. As the temperature of proto-Sun rose high enough to ignite thermo-nuclear reactions, some bodies inside the disk began to grow by collision and ...
Planetary system formation in thermally evolving viscous
... The above planets have been discovered largely from radial-velocity and/or transit surveys. Microlensing discoveries suggest the existence of both high- and low-mass planets orbiting at intermediate distance from their stars [5], whereas direct imaging surveys are beginning to uncover a population o ...
... The above planets have been discovered largely from radial-velocity and/or transit surveys. Microlensing discoveries suggest the existence of both high- and low-mass planets orbiting at intermediate distance from their stars [5], whereas direct imaging surveys are beginning to uncover a population o ...
Planets can alter each other`s climates over eons
... exoplanets is still at an early stage, our instruments are biased towards detecting planets that closely orbit their host stars. As a result, many of these multi-planet systems we know of look like scrunched-up versions of our solar system. These compact solar systems often have several planets whir ...
... exoplanets is still at an early stage, our instruments are biased towards detecting planets that closely orbit their host stars. As a result, many of these multi-planet systems we know of look like scrunched-up versions of our solar system. These compact solar systems often have several planets whir ...
Protostellar/PMS Mass Infall Luminosity Problem
... The infall rate of the secondary grows by 2–3 orders of magnitude at the approximate time of the periastro, becoming comparable to the infall rate of the primary. ...
... The infall rate of the secondary grows by 2–3 orders of magnitude at the approximate time of the periastro, becoming comparable to the infall rate of the primary. ...
shirley - Yancy L. Shirley`s Webpage
... What is the relative importance of spontaneous and stimulated processes in the formation of stars of various mass? What governs the SFR in a molecular cloud? What determined the IMF evolution from molecular cloud clumps to stars? Do stars form in a process of fragmentation of an overall collapse? Or ...
... What is the relative importance of spontaneous and stimulated processes in the formation of stars of various mass? What governs the SFR in a molecular cloud? What determined the IMF evolution from molecular cloud clumps to stars? Do stars form in a process of fragmentation of an overall collapse? Or ...
Lec9_2D
... The gravity at the surface of a red giant star is extremely weak. Any excess motion in the stellar atmosphere can cause the star to lose its mass into space. During this phase, stars can lose a lot of mass. ...
... The gravity at the surface of a red giant star is extremely weak. Any excess motion in the stellar atmosphere can cause the star to lose its mass into space. During this phase, stars can lose a lot of mass. ...
Lecture 3 - Minimum mass model of solar nebula
... Surface density of disk near Mercury is therefore: 1160x1026 / 1.82 x 1026 = 637 g cm-2 ...
... Surface density of disk near Mercury is therefore: 1160x1026 / 1.82 x 1026 = 637 g cm-2 ...
01 - Ionia Public Schools
... 11. What is important about the onset of fusion? _______________________________________________________________ _______________________________________________________________ 12. What happens as gravity increases the pressure on the matter within a star? ___________________________________________ ...
... 11. What is important about the onset of fusion? _______________________________________________________________ _______________________________________________________________ 12. What happens as gravity increases the pressure on the matter within a star? ___________________________________________ ...
Russell County Schools Non-Traditional Instructional Expectations
... very dense plasma forms. If the initial star had mass of less than 1.4 solar masses (1.4 times the mass of our sun), the process ceases at the density of 1,000 tons per cubic inch, and the star becomes the white dwarf. However, if the star was originally more massive, the white dwarf plasma can’t re ...
... very dense plasma forms. If the initial star had mass of less than 1.4 solar masses (1.4 times the mass of our sun), the process ceases at the density of 1,000 tons per cubic inch, and the star becomes the white dwarf. However, if the star was originally more massive, the white dwarf plasma can’t re ...
Solar System Formation Reading
... objects, protoplanets. Quite quickly (in less than 100 million years - that's short compared to the 4.5 billion year age of the solar system) the collision and coalescence leads to a few large objects that orbit in roughly circular orbits, with a fair amount of junk in between. At some point all of ...
... objects, protoplanets. Quite quickly (in less than 100 million years - that's short compared to the 4.5 billion year age of the solar system) the collision and coalescence leads to a few large objects that orbit in roughly circular orbits, with a fair amount of junk in between. At some point all of ...
Main Sequence Stars
... • Spheres of water have several properties: mass, volume, radius, surface area … • We can make a “Vogt-Russell” theorem for balls of water that says that all of the other properties of a ball of water are determined by just the mass and even write down equations, i.e. volume = mass/(density of water ...
... • Spheres of water have several properties: mass, volume, radius, surface area … • We can make a “Vogt-Russell” theorem for balls of water that says that all of the other properties of a ball of water are determined by just the mass and even write down equations, i.e. volume = mass/(density of water ...