Test#4
... 18. The reason the Solar system does not have a lot of dust and gas between the planets is a) the solar wind blew the dust and gas out of the Solar system b) the planets accreted all the gas and dust c) the early Solar system was made up only of Hydrogen and Helium d) the Sun burns them up 19. All ...
... 18. The reason the Solar system does not have a lot of dust and gas between the planets is a) the solar wind blew the dust and gas out of the Solar system b) the planets accreted all the gas and dust c) the early Solar system was made up only of Hydrogen and Helium d) the Sun burns them up 19. All ...
Agenda - Relativity Group
... a. Yes, all stars create heavier elements than carbon when they become a supernova. b. Yes, but there would be far fewer heavier elements because high-mass stars form elements like iron far more prolifically than low-mass stars. c. No, the core temperatures of low-mass stars are too low to fuse othe ...
... a. Yes, all stars create heavier elements than carbon when they become a supernova. b. Yes, but there would be far fewer heavier elements because high-mass stars form elements like iron far more prolifically than low-mass stars. c. No, the core temperatures of low-mass stars are too low to fuse othe ...
Chapter 19 Star Formation
... But interstellar molecular clouds are enormous, often containing up to a million solar masses of gas (and 1% dust--it is just part of the ISM. That is a lot of self-gravity! The most massive clouds have gravity that can overcome the thermal pressure trying to resist gravity, and the cloud must colla ...
... But interstellar molecular clouds are enormous, often containing up to a million solar masses of gas (and 1% dust--it is just part of the ISM. That is a lot of self-gravity! The most massive clouds have gravity that can overcome the thermal pressure trying to resist gravity, and the cloud must colla ...
Document
... through an accretion disk • As the matter gets closer to the object, it moves faster and gets hotter because of friction, and produces X-rays • Nova: the detonation of accumulated hydrogen in an accretion disk around a white dwarf • Type 1a Supernova: collapse and explosion of a white dwarf that has ...
... through an accretion disk • As the matter gets closer to the object, it moves faster and gets hotter because of friction, and produces X-rays • Nova: the detonation of accumulated hydrogen in an accretion disk around a white dwarf • Type 1a Supernova: collapse and explosion of a white dwarf that has ...
Chapter 15 Stars, Galaxies
... d. Black Hole e. Stars that are the most massive become black holes. Stars that are less massive but still high-mass stars become neutron stars. f. They all start out as a part of nebulas that contract to form protostars. g. Low-mass and medium-mass stars turn into red giants as they use up their fu ...
... d. Black Hole e. Stars that are the most massive become black holes. Stars that are less massive but still high-mass stars become neutron stars. f. They all start out as a part of nebulas that contract to form protostars. g. Low-mass and medium-mass stars turn into red giants as they use up their fu ...
Ch. 19 (Starbirth)
... The main sequence is a band, rather than a line, because stars of the same mass can have different compositions. Most important: Stars do not move along the main sequence! Once they reach it, they are in equilibrium, and do not move until their fuel begins to run out. ...
... The main sequence is a band, rather than a line, because stars of the same mass can have different compositions. Most important: Stars do not move along the main sequence! Once they reach it, they are in equilibrium, and do not move until their fuel begins to run out. ...
Document
... Earth has Newtonian Physics; BHs have Relativistic Physics if you ride into a BH you go in if you watch someone ride in they stay at Rs ...
... Earth has Newtonian Physics; BHs have Relativistic Physics if you ride into a BH you go in if you watch someone ride in they stay at Rs ...
Part B
... No fusion in white dwarf, star is supported only by electron degeneracy pressure. This sets max mass for a white dwarf, Chandrasekhar limit, at approximately 1.4 solar masses. Beyond this it cannot be supported by degeneracy pressure alone. Type I supernova occurs when white dwarf acquires additiona ...
... No fusion in white dwarf, star is supported only by electron degeneracy pressure. This sets max mass for a white dwarf, Chandrasekhar limit, at approximately 1.4 solar masses. Beyond this it cannot be supported by degeneracy pressure alone. Type I supernova occurs when white dwarf acquires additiona ...
Chapter 17 Star Stuff Agenda How does a star`s mass affect nuclear
... Thought Question The binary star Algol consists of a 3.7 MSun main sequence star and a 0.8 MSun subgiant star. ...
... Thought Question The binary star Algol consists of a 3.7 MSun main sequence star and a 0.8 MSun subgiant star. ...
Supernovae
... • Thus a stalled shock wave is revived by neutrino heating. • Boundary at ~150 km: – inside → matter falls into core – outside → matter is expelled. ...
... • Thus a stalled shock wave is revived by neutrino heating. • Boundary at ~150 km: – inside → matter falls into core – outside → matter is expelled. ...
Lecture 15 Star Formation and Evolution 3/7
... not Red Giant White Dwarf Red GiantWhite Dwarf Supernova: neutron star Supernova: black hole PHYS 162 ...
... not Red Giant White Dwarf Red GiantWhite Dwarf Supernova: neutron star Supernova: black hole PHYS 162 ...
Star Show FACILITATOR NOTES
... closely matches the Sun’s spectrum must have a temperature very close to the temperature at the Sun’s visible surface—well over 5000°C. Except for specialized lights used in photography, most real light filaments operate at a lower temperature (around 2500°C) which gives a more reddish-orange color ...
... closely matches the Sun’s spectrum must have a temperature very close to the temperature at the Sun’s visible surface—well over 5000°C. Except for specialized lights used in photography, most real light filaments operate at a lower temperature (around 2500°C) which gives a more reddish-orange color ...
Life Cycle of a Star - Intervention Worksheet
... _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a nebula _____ What happens next depends on the mass of the star. _____ Heat and pressure ...
... _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a nebula _____ What happens next depends on the mass of the star. _____ Heat and pressure ...
Lecture 33
... synthesized in the Big Bang theory were a prediction, but it was immediately realized that this explained why so much of the interstellar material is H and He. • What about the other elements? ...
... synthesized in the Big Bang theory were a prediction, but it was immediately realized that this explained why so much of the interstellar material is H and He. • What about the other elements? ...
10.1 The Solar Neighborhood Barnard`s Star
... Stellar spectra are much more informative than the blackbody curves. There are seven general categories of stellar spectra, corresponding to different ...
... Stellar spectra are much more informative than the blackbody curves. There are seven general categories of stellar spectra, corresponding to different ...
Lecture 16
... and transport of energy by convection. Those equations will not be discussed in this course. It is sufficient to know that they exist, and allow a complete solution to the structure of stars. Normally the equations of stellar structure are expressed as a set of coupled differential equations. They a ...
... and transport of energy by convection. Those equations will not be discussed in this course. It is sufficient to know that they exist, and allow a complete solution to the structure of stars. Normally the equations of stellar structure are expressed as a set of coupled differential equations. They a ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.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.