Comparing Earth, Sun and Jupiter
... Energy is transported to the surface via either radiation or convection. The Sun has a convective envelope and radiative interior. Low mass main-sequence stars are entirely convective. More massive stars are much more luminous (the fusion reactions release much more energy) Therefore they bu ...
... Energy is transported to the surface via either radiation or convection. The Sun has a convective envelope and radiative interior. Low mass main-sequence stars are entirely convective. More massive stars are much more luminous (the fusion reactions release much more energy) Therefore they bu ...
M What is the emptiness before the Big Bang? R Read the variables
... this area where gravity is so strong that nothing can exist, not even light? ...
... this area where gravity is so strong that nothing can exist, not even light? ...
Interstellar clouds
... 9% Helium, and 1% dust grains. • It has an extremely low density of 1 atom per cm3, about 10 billionth the density of gas created by our best vacuums here on earth. ...
... 9% Helium, and 1% dust grains. • It has an extremely low density of 1 atom per cm3, about 10 billionth the density of gas created by our best vacuums here on earth. ...
Study Notes for Chapter 30: Stars, Galaxies, and the Universe
... 2. A large, bright star whose hot core has used most of its hydrogen is a nova. 3. A light-year is the distance light travels in a year. 4. A small, hot, extremely dense core left after a star collapses is a white dwarf. 5. A star moving away from the Earth has a spectrum that is shifted toward red. ...
... 2. A large, bright star whose hot core has used most of its hydrogen is a nova. 3. A light-year is the distance light travels in a year. 4. A small, hot, extremely dense core left after a star collapses is a white dwarf. 5. A star moving away from the Earth has a spectrum that is shifted toward red. ...
PHYS3380_102615_bw
... We have observed disks around other stars. These could be new planetary systems in formation. ...
... We have observed disks around other stars. These could be new planetary systems in formation. ...
Stars and Black Holes: Stars A star is a massive, luminous ball of
... There are _____________ of galaxies in the ______________. Galaxies are ________________: they contain ________, ___________, and _______. The farthest galaxies and the stars we see shining in them may be also the _____________ because it takes the _____________ so long to reach us. ...
... There are _____________ of galaxies in the ______________. Galaxies are ________________: they contain ________, ___________, and _______. The farthest galaxies and the stars we see shining in them may be also the _____________ because it takes the _____________ so long to reach us. ...
Protostars and planets
... higher than the entropy of a main-sequence star of the same mass. As entropy is lost to radiation and the radius contracts, the central temperature rises until the thermonuclear reaction rate balances the luminosity. At this point the protostar joins the zero-age main sequence (ZAMS). The astronomic ...
... higher than the entropy of a main-sequence star of the same mass. As entropy is lost to radiation and the radius contracts, the central temperature rises until the thermonuclear reaction rate balances the luminosity. At this point the protostar joins the zero-age main sequence (ZAMS). The astronomic ...
Physical properties of stars
... that are 1,000 times larger than our sun. pg. 450 Temperature: Surface temperatures range from 3000K to 30,000K Color is an indication of temperature. Blue hottest White Yellow Orange Red coolest Mass While the size of stars varies widely the mass does not. 15 times our Sun’s mass to .2 times our Su ...
... that are 1,000 times larger than our sun. pg. 450 Temperature: Surface temperatures range from 3000K to 30,000K Color is an indication of temperature. Blue hottest White Yellow Orange Red coolest Mass While the size of stars varies widely the mass does not. 15 times our Sun’s mass to .2 times our Su ...
Lifecycle of Stars - Mrs. Plante Science
... • GRAVITY causes this gas and dust to come together, forming larger and larger balls of gas and dust molecules. • When the mass becomes large enough, gravitational contraction results in high pressure and temperature, and a protostar is formed. ...
... • GRAVITY causes this gas and dust to come together, forming larger and larger balls of gas and dust molecules. • When the mass becomes large enough, gravitational contraction results in high pressure and temperature, and a protostar is formed. ...
New Directions in Star Cluster Research
... Astrophysics (physics of stars) Is not an experimental science - we cannot devise and conduct experiments in order to test theories Theory is validated by observations Evidence often derived from past events Information we can gather is very restricted - apparent brightness (depends on distance), l ...
... Astrophysics (physics of stars) Is not an experimental science - we cannot devise and conduct experiments in order to test theories Theory is validated by observations Evidence often derived from past events Information we can gather is very restricted - apparent brightness (depends on distance), l ...
Astronomy - Shelbyville Central Schools
... Stars differ in composition, age, and size. *young stars are rich in hydrogen *older stars use up hydrogen to produce more helium ...
... Stars differ in composition, age, and size. *young stars are rich in hydrogen *older stars use up hydrogen to produce more helium ...
lecture20
... collapse. • As more gas fell in, it’s potential energy was converted into thermal energy. • Eventually the in-falling gas was hot enough to ignite nuclear fusion in the core. • Gas that continued to fall in helped to establish gravitational equilibrium with the pressure generated in the core. ...
... collapse. • As more gas fell in, it’s potential energy was converted into thermal energy. • Eventually the in-falling gas was hot enough to ignite nuclear fusion in the core. • Gas that continued to fall in helped to establish gravitational equilibrium with the pressure generated in the core. ...
A Star is Born!
... the gas increase → more blackbody radiation • Opacity — the gas is not transparent to the radiation, and the radiation interacts with the gas particles exerting an outward pressure known as radiation pressure ...
... the gas increase → more blackbody radiation • Opacity — the gas is not transparent to the radiation, and the radiation interacts with the gas particles exerting an outward pressure known as radiation pressure ...
Study Notes for Chapter 30:
... A star with the sun’s mass would stay on the _____ sequence of the H-R diagram for about 10 billion years. ...
... A star with the sun’s mass would stay on the _____ sequence of the H-R diagram for about 10 billion years. ...
Lecture 14: Star Formation
... a lot from observations of protostars and pre-main sequence stars in different stages of formation. We can learn both what they look like, and, from the number that we see, an idea of how long the various stages last. ...
... a lot from observations of protostars and pre-main sequence stars in different stages of formation. We can learn both what they look like, and, from the number that we see, an idea of how long the various stages last. ...
![Lectures 10 & 11 powerpoint (stellar formation) [movie below]](http://s1.studyres.com/store/data/008083226_1-fec717da713794a7feea61d4eec0ceb1-300x300.png)
Lectures 10 & 11 powerpoint (stellar formation) [movie below]
... gas can remain ionized because of very low density. ...
... gas can remain ionized because of very low density. ...
Star Formation
... it picks up speed and energy. It is slowed by friction and the energy is converted to heat. ...
... it picks up speed and energy. It is slowed by friction and the energy is converted to heat. ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.