Review 1 Solutions
... 7. Jupiter’s moon Callisto has lots and lots of craters, whereas another moon, Io, has almost none. What does this tell us about Io and Callisto? Io has a younger surface than Callisto. From other observations, we know this is because of volcanic activity on Io that constantly replenishes its surfac ...
... 7. Jupiter’s moon Callisto has lots and lots of craters, whereas another moon, Io, has almost none. What does this tell us about Io and Callisto? Io has a younger surface than Callisto. From other observations, we know this is because of volcanic activity on Io that constantly replenishes its surfac ...
Stellar Evolution – Life of a Star
... EQUILIBRIUM. The liberation of energy from the interior of the star is balanced by the energy released at the surface of the star. The energy is produced by hydrogen burning in the core of star (conversion by fusion of H to He). • A second property is HYDROSTATIC EQUILIBRIUM. There is sufficient pre ...
... EQUILIBRIUM. The liberation of energy from the interior of the star is balanced by the energy released at the surface of the star. The energy is produced by hydrogen burning in the core of star (conversion by fusion of H to He). • A second property is HYDROSTATIC EQUILIBRIUM. There is sufficient pre ...
Ch. 27.3 Star Groups
... One complete rotation in 200 million years. Our sun is about 30,000 light-years from the center. ...
... One complete rotation in 200 million years. Our sun is about 30,000 light-years from the center. ...
Chapter 19 Star Formation
... 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. ...
... 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. ...
Stars!!!!
... – Created from small and medium stars – When they run out of fuel the expand to a red giant – These gases eventually blow away leaving the blue white core – They are about the size of Earth but with the mass of the sun – When it dies it is called a black dwarf ...
... – Created from small and medium stars – When they run out of fuel the expand to a red giant – These gases eventually blow away leaving the blue white core – They are about the size of Earth but with the mass of the sun – When it dies it is called a black dwarf ...
Stellar Evolution
... core is almost totally due to “electron degeneracy” – two electrons cannot be in the same quantum state, so the core cannot contract beyond a certain point. This pressure is almost independent of temperature – when the helium starts fusing, the pressure cannot adjust. Helium begins to fuse extre ...
... core is almost totally due to “electron degeneracy” – two electrons cannot be in the same quantum state, so the core cannot contract beyond a certain point. This pressure is almost independent of temperature – when the helium starts fusing, the pressure cannot adjust. Helium begins to fuse extre ...
Lecture 26 - Empyrean Quest Publishers
... 1. Dust--recycled star material. Light undergoes to changes in going through it (Trumpler 1930): A. reddening--preferential scattering-blue light (why sky is blue). B. absorption--this affects flux and measured distance. 2. Molecular Clouds--H2 molecules--dense MC are star formation regions (stellar ...
... 1. Dust--recycled star material. Light undergoes to changes in going through it (Trumpler 1930): A. reddening--preferential scattering-blue light (why sky is blue). B. absorption--this affects flux and measured distance. 2. Molecular Clouds--H2 molecules--dense MC are star formation regions (stellar ...
Chapter 40
... – Older stars had only hydrogen and helium – Elements heavier than hydrogen and helium came from the core of stars – When stars die, they spew material out – Newer stars are composed of heavier elements – We are made of star dust! ...
... – Older stars had only hydrogen and helium – Elements heavier than hydrogen and helium came from the core of stars – When stars die, they spew material out – Newer stars are composed of heavier elements – We are made of star dust! ...
Chapter 13
... History of Stellar Evolution Theories • Aristotle wrote more than 2000 years ago that stars are heated by their passage through the heavens, but never considered that they evolved • In the 18th century, Immanuel Kant described the Sun as a fiery sphere, formed from the gases gravitated to the cente ...
... History of Stellar Evolution Theories • Aristotle wrote more than 2000 years ago that stars are heated by their passage through the heavens, but never considered that they evolved • In the 18th century, Immanuel Kant described the Sun as a fiery sphere, formed from the gases gravitated to the cente ...
Stars and Galaxies – Notes
... Steps for the “birth” of stars: o Large clouds of gas and dust, called nebulae, collapse due to gravity. o The collapsing cloud becomes very dense. o Nuclear reactions involving hydrogen and helium begin. o These nuclear reactions power the star. o A star is born. ...
... Steps for the “birth” of stars: o Large clouds of gas and dust, called nebulae, collapse due to gravity. o The collapsing cloud becomes very dense. o Nuclear reactions involving hydrogen and helium begin. o These nuclear reactions power the star. o A star is born. ...
Document
... Neutrons (and protons) are made of quarks. Gravity could crush neutrons into free quarks. Called strange matter (a type of quark). Astronomers think they may have seen a quark star. ...
... Neutrons (and protons) are made of quarks. Gravity could crush neutrons into free quarks. Called strange matter (a type of quark). Astronomers think they may have seen a quark star. ...
To understand the deaths of stars and how it depends on
... Time table • This all occurs in a time frame of about a week. • We have never been able to be lucky enough to watch a star go through this rapid transition. ...
... Time table • This all occurs in a time frame of about a week. • We have never been able to be lucky enough to watch a star go through this rapid transition. ...
PowerPoint - Chandra X
... The young Sun-like stars in Orion produce violent X-ray outbursts, or flares, that are much more frequent and energetic than anything seen today from our Sun. The range of flare energies is large, with some of the stars producing flares that are a hundred times larger than others. The different flar ...
... The young Sun-like stars in Orion produce violent X-ray outbursts, or flares, that are much more frequent and energetic than anything seen today from our Sun. The range of flare energies is large, with some of the stars producing flares that are a hundred times larger than others. The different flar ...
![Chapter Zero Section 0.2 [reprint from Jesperson 7th] Supernovas](http://s1.studyres.com/store/data/009810478_1-e5fd9db32afbb84e749a32319c4308af-300x300.png)
Chapter Zero Section 0.2 [reprint from Jesperson 7th] Supernovas
... As the stars grew in size, the temperature and pressure within each star increased to the point where nuclear fusion of hydrogen nuclei into helium started and stars began to shine. Heat generated from the fusion of hydrogen to helium maintained the volume and pressure within a star for millions of ...
... As the stars grew in size, the temperature and pressure within each star increased to the point where nuclear fusion of hydrogen nuclei into helium started and stars began to shine. Heat generated from the fusion of hydrogen to helium maintained the volume and pressure within a star for millions of ...
Chapter 13
... activity • Intense outward gas flows from surfaces • Occupy H-R diagram just above main-sequence ...
... activity • Intense outward gas flows from surfaces • Occupy H-R diagram just above main-sequence ...
Assignment 8 - utoledo.edu
... a. their outer envelopes expand significantly b. they lose a significant amount of mass from their outside layers c. their surface temperatures become lower than before d. their overall luminosities increase e. their mass grows significantly as they incorporate planets and interstellar matter near t ...
... a. their outer envelopes expand significantly b. they lose a significant amount of mass from their outside layers c. their surface temperatures become lower than before d. their overall luminosities increase e. their mass grows significantly as they incorporate planets and interstellar matter near t ...
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.