The Milky Way - Houston Community College System
... A. Star Birth in Giant Molecular Clouds B. Heating By Contraction C. Protostars II. The Orion Nebula: Evidence of Star Formation A. Observing Star Formation B. Contagious Star Formation III. Young Stellar Objects and Protostellar Disks ...
... A. Star Birth in Giant Molecular Clouds B. Heating By Contraction C. Protostars II. The Orion Nebula: Evidence of Star Formation A. Observing Star Formation B. Contagious Star Formation III. Young Stellar Objects and Protostellar Disks ...
What We Know About Stars So Far
... use up their energy and lose mass. • Smaller, cooler stars burn their fuel slowly and last longer • Massive, supergiant stars burn their fuel quickly and don’t last as long. The loss of mass in a star creates a stellar wind (called solar wind in the case of our Sun). ...
... use up their energy and lose mass. • Smaller, cooler stars burn their fuel slowly and last longer • Massive, supergiant stars burn their fuel quickly and don’t last as long. The loss of mass in a star creates a stellar wind (called solar wind in the case of our Sun). ...
QUIZ 1 - AY5-S13 . . . . . . . . . . . . . . . . . YOUR NAME
... 7. Suppose you lived on the Moon where there is essentially no atmosphere. Label the following statements as (T)rue or (F)alse: F The Sun would appear redder (compared to as seen from the Earth) during the day. T The color of the sky (looking away from the Sun during the day) would be black. F At su ...
... 7. Suppose you lived on the Moon where there is essentially no atmosphere. Label the following statements as (T)rue or (F)alse: F The Sun would appear redder (compared to as seen from the Earth) during the day. T The color of the sky (looking away from the Sun during the day) would be black. F At su ...
Chapter 2 Basic Chemistry
... • Massive Stars evolve faster than smaller Stars – The formation of an iron core signals the beginning of a supergiant Star’s death because, unlike fusing lighter elements, fusing iron atoms to make heavier elements requires adding energy rather than releasing it – When fusion requires more energy t ...
... • Massive Stars evolve faster than smaller Stars – The formation of an iron core signals the beginning of a supergiant Star’s death because, unlike fusing lighter elements, fusing iron atoms to make heavier elements requires adding energy rather than releasing it – When fusion requires more energy t ...
Part 1, Some Basics
... temperature) to bottom-right (low luminosity and low surface temperature) – 90% stars in this band – The Sun is one of main sequence stars – Hydrogen burning as energy source ...
... temperature) to bottom-right (low luminosity and low surface temperature) – 90% stars in this band – The Sun is one of main sequence stars – Hydrogen burning as energy source ...
iptfsummer2014bildsten
... so that the <2M primary fills the Roche lobe on the first ascent of the red giant branch will have a degenerate He core of mass 0.150.48 M • Large orbital period range relevant for this to occur, from a few days to over a year. ...
... so that the <2M primary fills the Roche lobe on the first ascent of the red giant branch will have a degenerate He core of mass 0.150.48 M • Large orbital period range relevant for this to occur, from a few days to over a year. ...
Slides from the second lecture
... In low-mass stars the core never gets hot enough to ignite Carbon-burning. However, the rate of He-burning in the shell source is unstable, so the star pulsates and the envelope of the star is ejected in a planetary nebula. The core of the star remains behind as a white dwarf star ...
... In low-mass stars the core never gets hot enough to ignite Carbon-burning. However, the rate of He-burning in the shell source is unstable, so the star pulsates and the envelope of the star is ejected in a planetary nebula. The core of the star remains behind as a white dwarf star ...
Astronomy 100 Name(s):
... Horrible fates 14. A star with the mass of Sirius A (16 solar masses) can end its “life” by undergoing a supernova. How long before the lethal front of x-rays and cosmic rays the supernova generates overwhelms the Earth? ...
... Horrible fates 14. A star with the mass of Sirius A (16 solar masses) can end its “life” by undergoing a supernova. How long before the lethal front of x-rays and cosmic rays the supernova generates overwhelms the Earth? ...
Astronomy 162 Lab 4: Stars
... White Dwarfs at the bottom. It turns out that Main Sequence stars are in the prime of their lives, those stars burning Hydrogen into Helium are found on the middle line. Giants and Super Giants are old stars burning the helium into carbon and other elements at the end of their lives. Finally, white ...
... White Dwarfs at the bottom. It turns out that Main Sequence stars are in the prime of their lives, those stars burning Hydrogen into Helium are found on the middle line. Giants and Super Giants are old stars burning the helium into carbon and other elements at the end of their lives. Finally, white ...
Astronomy 15 - Problem Set Number 7
... for rough purposes. Find an expression for the average density of a mass M which is compressed to just its Schwarzschild radius; now evaluate it numerically to show that the average density 1.8 × 1016 gm cm−3 ρ̄ = mass in solar masses If a mass is compressed beyond this density, it will surely be un ...
... for rough purposes. Find an expression for the average density of a mass M which is compressed to just its Schwarzschild radius; now evaluate it numerically to show that the average density 1.8 × 1016 gm cm−3 ρ̄ = mass in solar masses If a mass is compressed beyond this density, it will surely be un ...
star life cycle
... Using the quiz … Click through the quiz to see the questions and answers. Remember it is MUCH better to try to think of the answer, before clicking to read it. ...
... Using the quiz … Click through the quiz to see the questions and answers. Remember it is MUCH better to try to think of the answer, before clicking to read it. ...
PowerPoint - Chandra X
... N132D is the remnant of a supernova explosion that occurred when the core of a massive star collapsed to form a neutron star or black hole (core-collapse supernova). The estimated age of the remnant is 3,000 years. Most of the oxygen in the universe is thought to be dispersed into space by core-coll ...
... N132D is the remnant of a supernova explosion that occurred when the core of a massive star collapsed to form a neutron star or black hole (core-collapse supernova). The estimated age of the remnant is 3,000 years. Most of the oxygen in the universe is thought to be dispersed into space by core-coll ...
ppt - Astronomy & Physics
... The mass of the Helium nucleus is less than the mass of the 4 protons, and this mass is converted into energy, which powers the Sun (and other stars) ...
... The mass of the Helium nucleus is less than the mass of the 4 protons, and this mass is converted into energy, which powers the Sun (and other stars) ...
CoRoT: a space project to listen to the songs of the stars
... CoRoT: a space satellite to listen to the songs of the stars CoRoT, an ambitious European space satellite, is going to be launched on December 27, 2006. Its main purpose is to study the interiors of the stars and to detect planets orbiting around the Sun-like stars (the acronym CoRoT stands for Conv ...
... CoRoT: a space satellite to listen to the songs of the stars CoRoT, an ambitious European space satellite, is going to be launched on December 27, 2006. Its main purpose is to study the interiors of the stars and to detect planets orbiting around the Sun-like stars (the acronym CoRoT stands for Conv ...
Chapter 10- Stars, Galaxies and the Universe
... 37. Telescopes work by collecting and focusing different forms of ____________________ radiation. 38. Astronomers can determine a star’s chemical composition by using a(n) _________________________ to observe the wavelengths of light the star emits. 39. The most massive stars collapse to form ______ ...
... 37. Telescopes work by collecting and focusing different forms of ____________________ radiation. 38. Astronomers can determine a star’s chemical composition by using a(n) _________________________ to observe the wavelengths of light the star emits. 39. The most massive stars collapse to form ______ ...
Lecture 14
... A protostar is the name we give a star that is just forming … i.e. it has not yet reached the main sequence. The initial disk that forms around the star is called a protostellar disk (also sometimes called a protoplanetary disk). ...
... A protostar is the name we give a star that is just forming … i.e. it has not yet reached the main sequence. The initial disk that forms around the star is called a protostellar disk (also sometimes called a protoplanetary disk). ...
document
... • A protostar contracts and heats until the core temperature is sufficient for hydrogen fusion. ...
... • A protostar contracts and heats until the core temperature is sufficient for hydrogen fusion. ...
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.