High-mass stars in the Galactic center Quintuplet cluster
... the luminous late-type WN stars (WNL) are an interphase between O stars leaving the main-sequence and WR stars of the carbon sequence (WC), before these massive stars explode as supernova (SN). As shown in the HRD (Fig. 4) the WNL stars in the Quintuplet form a group of relatively cool but very lumi ...
... the luminous late-type WN stars (WNL) are an interphase between O stars leaving the main-sequence and WR stars of the carbon sequence (WC), before these massive stars explode as supernova (SN). As shown in the HRD (Fig. 4) the WNL stars in the Quintuplet form a group of relatively cool but very lumi ...
Astrophysics - Part 2
... higher will be its absolute magnitude and surface temperature but the shorter is the time the star remains MAIN SEQUENCE. The Sun is about half-way through its 10 billion year passage. The largest stars may only last for tens of millions of years. While on the MAIN SEQUENCE the star’s absolute magni ...
... higher will be its absolute magnitude and surface temperature but the shorter is the time the star remains MAIN SEQUENCE. The Sun is about half-way through its 10 billion year passage. The largest stars may only last for tens of millions of years. While on the MAIN SEQUENCE the star’s absolute magni ...
hotstar_xrays
... scorpion -- as seen at 10 PM on a June evening from Swarthmore. t Sco is a B0 V star -- with a surface temperature of about 30,000 K (5 times the sun’s temperature), and with about 50,000 times the sun’s luminosity. It has unusual ultraviolet absorption lines, a very low projected rotational velocit ...
... scorpion -- as seen at 10 PM on a June evening from Swarthmore. t Sco is a B0 V star -- with a surface temperature of about 30,000 K (5 times the sun’s temperature), and with about 50,000 times the sun’s luminosity. It has unusual ultraviolet absorption lines, a very low projected rotational velocit ...
Pp 263-266 - Gravity From The Ground Up
... We have learned that neutron stars can only exist in a rather restricted range of masses, between perhaps 0.1 and two solar masses. In fact, their lower limit in practice will normally be much larger, since a collapsing star will stop at the white dwarf stage if its mass is less than the Chandrasekh ...
... We have learned that neutron stars can only exist in a rather restricted range of masses, between perhaps 0.1 and two solar masses. In fact, their lower limit in practice will normally be much larger, since a collapsing star will stop at the white dwarf stage if its mass is less than the Chandrasekh ...
Activity Book Level 4
... planets, called the gas giants, are significantly more massive than the terrestrials. The two largest, Jupiter and Saturn, are made mainly of hydrogen and helium. The two outermost planets, Uranus and Neptune, are made largely of substances with relatively high melting points called ices, such as wa ...
... planets, called the gas giants, are significantly more massive than the terrestrials. The two largest, Jupiter and Saturn, are made mainly of hydrogen and helium. The two outermost planets, Uranus and Neptune, are made largely of substances with relatively high melting points called ices, such as wa ...
Nuclear Fusion - Orlando STC chapter
... Ever since the beginning of life on Earth, the Sun has sent the energy needed to keep its inhabitants alive. Solar rays light the days, warm the soil, and provide plants with the raw energy they need to make food. We know the Earth’s energy comes from the Sun, but from where does the Sun’s energy ...
... Ever since the beginning of life on Earth, the Sun has sent the energy needed to keep its inhabitants alive. Solar rays light the days, warm the soil, and provide plants with the raw energy they need to make food. We know the Earth’s energy comes from the Sun, but from where does the Sun’s energy ...
27B Star Life Cycle and the HR Diagram
... d. Which stars on your graph are located in the area associated with white dwarf stars? ...
... d. Which stars on your graph are located in the area associated with white dwarf stars? ...
Animated Planets PowerPoint Presentation
... of planetary nebulae, their central stars and how planetary nebulae fit into the patterns of stellar evolution. She also analyzes the spectra of symbiotic stars (binaries containing an evolved hot star and a cool star) to determine their chemical compositions, velocities and variability. ...
... of planetary nebulae, their central stars and how planetary nebulae fit into the patterns of stellar evolution. She also analyzes the spectra of symbiotic stars (binaries containing an evolved hot star and a cool star) to determine their chemical compositions, velocities and variability. ...
Chapter 8 powerpoint presentation
... How many of the H atoms are in each of the excitation levels, n=1, n=2, etc, described by the Boltzmann equation and secondly, how many of the H atoms are completely ionized, for if the H atoms are ionized they can not produce any absorption lines. This is described by the Saha equation. ...
... How many of the H atoms are in each of the excitation levels, n=1, n=2, etc, described by the Boltzmann equation and secondly, how many of the H atoms are completely ionized, for if the H atoms are ionized they can not produce any absorption lines. This is described by the Saha equation. ...
ASTR 1101-001 Spring 2008 - Louisiana State University
... • Astronomers determine the mass of a star by examining how strong the gravitational field is around that star. (Isaac Newton’s law of universal gravitation; §4-7) • By studying the motion of planets around our Sun, astronomers have determined that the Sun has a mass of 2 x 1030 kilograms. • We cann ...
... • Astronomers determine the mass of a star by examining how strong the gravitational field is around that star. (Isaac Newton’s law of universal gravitation; §4-7) • By studying the motion of planets around our Sun, astronomers have determined that the Sun has a mass of 2 x 1030 kilograms. • We cann ...
Planisphere Exercise
... planisphere. As the night progresses, which way do the stars appear to move around the North Star (which is hidden under the brass fastener) – clockwise or counterclockwise? As the night progresses, how do stars appear to move across the southern sky? In what direction does the celestial equator app ...
... planisphere. As the night progresses, which way do the stars appear to move around the North Star (which is hidden under the brass fastener) – clockwise or counterclockwise? As the night progresses, how do stars appear to move across the southern sky? In what direction does the celestial equator app ...
Astronomy Exam #4
... C. Star α appears brighter that star γ. D. Star α is larger in radius than star γ. 14. Which statement is the most correct about the comparison between a K5 main sequence star and a B5 main sequence star? A. The K5 star is cooler, less luminous, smaller, and will not live as long as the B5 main sequ ...
... C. Star α appears brighter that star γ. D. Star α is larger in radius than star γ. 14. Which statement is the most correct about the comparison between a K5 main sequence star and a B5 main sequence star? A. The K5 star is cooler, less luminous, smaller, and will not live as long as the B5 main sequ ...
ExamView - es S1 dept final.tst
... a. by sampling matter on the surface of stars. b. by analyzing the vibrations that stars emit. c. through magnetic testing. d. by analyzing the spectra of the light that stars emit. 44. A small, hot, extremely dense core left after a star collapses is a a. red giant. c. black dwarf. b. pulsar. d. wh ...
... a. by sampling matter on the surface of stars. b. by analyzing the vibrations that stars emit. c. through magnetic testing. d. by analyzing the spectra of the light that stars emit. 44. A small, hot, extremely dense core left after a star collapses is a a. red giant. c. black dwarf. b. pulsar. d. wh ...
Jeans Length
... N molecules of mass m in box of size L at temp T. • Gravitational Energy: EG ~ G M M L ...
... N molecules of mass m in box of size L at temp T. • Gravitational Energy: EG ~ G M M L ...
1705 chart front
... them orbit around their parent planet. If you have trouble steadying your binocular view on Jupiter, try leaning them up against the side of a building or another steady surface. A small telescope not only shows the moons of Jupiter, but also its cloud bands. Jupiter has stripes! Look for our own Mo ...
... them orbit around their parent planet. If you have trouble steadying your binocular view on Jupiter, try leaning them up against the side of a building or another steady surface. A small telescope not only shows the moons of Jupiter, but also its cloud bands. Jupiter has stripes! Look for our own Mo ...
How do we know what stars are
... as the star ages. When helium begins to fuse together, elements like ____________ and ___________ appear in the spectrum. Heavier and heavier elements will be formed as the core runs out of hydrogen and helium. Stars cannot fuse atoms larger than the element __________. Toward the end of the life of ...
... as the star ages. When helium begins to fuse together, elements like ____________ and ___________ appear in the spectrum. Heavier and heavier elements will be formed as the core runs out of hydrogen and helium. Stars cannot fuse atoms larger than the element __________. Toward the end of the life of ...
What is a star?
... • Two or more stars may be bound together by gravity, which causes them to orbit each other. • Three or more stars that are bound by gravity are called multiple stars or multiple star systems. ...
... • Two or more stars may be bound together by gravity, which causes them to orbit each other. • Three or more stars that are bound by gravity are called multiple stars or multiple star systems. ...
Chapter 22 Neutron Stars and Black Holes
... Neutron stars, although they have 1–3 solar masses, are so dense that they are very small. This image shows a 1-solar-mass neutron star, about 10 km in diameter, compared to Manhattan: ...
... Neutron stars, although they have 1–3 solar masses, are so dense that they are very small. This image shows a 1-solar-mass neutron star, about 10 km in diameter, compared to Manhattan: ...
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.