HOU Supernova Light Curves
... In the spring of 1994 several HOU students were studying M51, the spiral galaxy also known as the Whirlpool Galaxy. Various HOU images had been requested throughout February and March, and in early April, two girls at Oil City High School in Pennsylvania received an important phone call. They had se ...
... In the spring of 1994 several HOU students were studying M51, the spiral galaxy also known as the Whirlpool Galaxy. Various HOU images had been requested throughout February and March, and in early April, two girls at Oil City High School in Pennsylvania received an important phone call. They had se ...
How do stars shine?
... After this step, its all downhill relatively speaking. It’s easy now to bump another proton into the deuterium to make Helium-3 - which is stable, the extra neutron acts as a sort of nuclear glue. This probably only takes a few seconds, compared to the billion of so for the first step. Then the next ...
... After this step, its all downhill relatively speaking. It’s easy now to bump another proton into the deuterium to make Helium-3 - which is stable, the extra neutron acts as a sort of nuclear glue. This probably only takes a few seconds, compared to the billion of so for the first step. Then the next ...
chapter15SurveyStars..
... • What is a Hertzsprung-Russell diagram? – An H-R diagram plots stellar luminosity of stars versus surface temperature (or color or spectral type) ...
... • What is a Hertzsprung-Russell diagram? – An H-R diagram plots stellar luminosity of stars versus surface temperature (or color or spectral type) ...
Astronomy 1020 Exam 4 Review Questions
... 1. What is meant by the asymptotic giant branch? Describe the interior structure of a star when it is on the AGB. 2. What is meant by dredge up and by thermal pulse ? 3. How are carbon stars made? 4. What is a planetary nebula? Why does such a nebula shine? 5. What are the differences between a deta ...
... 1. What is meant by the asymptotic giant branch? Describe the interior structure of a star when it is on the AGB. 2. What is meant by dredge up and by thermal pulse ? 3. How are carbon stars made? 4. What is a planetary nebula? Why does such a nebula shine? 5. What are the differences between a deta ...
Presentation - Harvard-Smithsonian Center for Astrophysics
... This stellar system consists of a red giant whose wind and surrounding nebula is photoionized by a hot white dwarf companion. Spectrum is complex with narrow nebular emission, and the surprising presencs of high ionization forbidden lines. These conditions are quite different from ‘coronal’ plasmas ...
... This stellar system consists of a red giant whose wind and surrounding nebula is photoionized by a hot white dwarf companion. Spectrum is complex with narrow nebular emission, and the surprising presencs of high ionization forbidden lines. These conditions are quite different from ‘coronal’ plasmas ...
Lesson 3 - The DK Foundation
... the comfort-loving personality, and never has been. It would not be spirituality if it were. Shamballa has said that only when we free ourselves from the pre-occupations of everyday life and rise up on the winds of inspiration, do we become visible to them. Until then we are indistinct like so many ...
... the comfort-loving personality, and never has been. It would not be spirituality if it were. Shamballa has said that only when we free ourselves from the pre-occupations of everyday life and rise up on the winds of inspiration, do we become visible to them. Until then we are indistinct like so many ...
Neutron Stars and Black Holes
... Black Holes in Galaxies • BHs may have formed in center when galaxy formed. • Mass of billions of stars in size of SS (Kepler’s 3rd Law). • Black hole likely in center of the Milky Way. ...
... Black Holes in Galaxies • BHs may have formed in center when galaxy formed. • Mass of billions of stars in size of SS (Kepler’s 3rd Law). • Black hole likely in center of the Milky Way. ...
presentation source
... “This, I imagine, is why the oldest members of the stellar system…are so large and populous, for the available material was richer then. As the layer of dust and gas sank toward the galactic plane, stars continued to form. Dust and gas still lie dense in this layer, and stars are still being formed ...
... “This, I imagine, is why the oldest members of the stellar system…are so large and populous, for the available material was richer then. As the layer of dust and gas sank toward the galactic plane, stars continued to form. Dust and gas still lie dense in this layer, and stars are still being formed ...
Stars A globular cluster is a tightly grouped swarm of stars held
... galaxy may be 100 billion. Thus, more than 10 billion trillion stars may exist. But if you look at the night sky far from city lights, you can see only about 3,000 of them without using binoculars or a telescope. Stars, like people, have life cycles -- they are born, pass through several phases, and ...
... galaxy may be 100 billion. Thus, more than 10 billion trillion stars may exist. But if you look at the night sky far from city lights, you can see only about 3,000 of them without using binoculars or a telescope. Stars, like people, have life cycles -- they are born, pass through several phases, and ...
Ch 3 PPT - Blountstown Middle School
... • After helium in the cores of lower-mass stars is gone, the stars cast off their gases, exposing their cores. • The core eventually becomes a white dwarf, a hot, dense, slowly cooling sphere of carbon. • This is what is expected to happen to the Sun. ...
... • After helium in the cores of lower-mass stars is gone, the stars cast off their gases, exposing their cores. • The core eventually becomes a white dwarf, a hot, dense, slowly cooling sphere of carbon. • This is what is expected to happen to the Sun. ...
Super Giant
... Explain why the moon revolves around the Earth instead of the Sun. Even though the moon is larger than Pluto, which DOES revolve around the Sun, The moon revolves around the Earth because it is CLOSER to the Earth. The two factors that determine the force of gravity are mass and distance. What relat ...
... Explain why the moon revolves around the Earth instead of the Sun. Even though the moon is larger than Pluto, which DOES revolve around the Sun, The moon revolves around the Earth because it is CLOSER to the Earth. The two factors that determine the force of gravity are mass and distance. What relat ...
about Stars
... Ages of Star Clusters The “bluest” stars left on the main sequence of the cluster tell us the cluster’s age. As the cluster ages, the bluest stars run out of hydrogen for fusion and lose their “shine” ...
... Ages of Star Clusters The “bluest” stars left on the main sequence of the cluster tell us the cluster’s age. As the cluster ages, the bluest stars run out of hydrogen for fusion and lose their “shine” ...
STScI 2005
... • Stars generally form with a frequency that decreases with increasing mass for masses greater than ~1 M: ...
... • Stars generally form with a frequency that decreases with increasing mass for masses greater than ~1 M: ...
The Milky Way Galaxy
... What is the remnant left over from a Type Ia (carbon detonation) supernova: A: a white dwarf + an expanding shell B: a neutron star + an expanding shell C: a black hole + an expanding shell D: no remnant, just the expanding shell ...
... What is the remnant left over from a Type Ia (carbon detonation) supernova: A: a white dwarf + an expanding shell B: a neutron star + an expanding shell C: a black hole + an expanding shell D: no remnant, just the expanding shell ...
CoRoT Observations of O Stars: Diverse Origins of Variability
... 2.3. HD 46966 (O8 V) Blomme et al. (2011) applied classical pre-whitening to the periodogram of HD 46966. About 300 frequencies are required before the noise level is reached. Significance tests show that all 300 frequencies are significant. It is, however, highly suspicious that so many pulsation f ...
... 2.3. HD 46966 (O8 V) Blomme et al. (2011) applied classical pre-whitening to the periodogram of HD 46966. About 300 frequencies are required before the noise level is reached. Significance tests show that all 300 frequencies are significant. It is, however, highly suspicious that so many pulsation f ...
Document
... High Mass Main Sequence Stars CNO cycle begins at 15 million degrees and becomes more dominant at higher temperatures. The C nucleus has a (+6) charge, so the incoming proton must be moving even faster to overcome the electromagnetic repulsion!! ...
... High Mass Main Sequence Stars CNO cycle begins at 15 million degrees and becomes more dominant at higher temperatures. The C nucleus has a (+6) charge, so the incoming proton must be moving even faster to overcome the electromagnetic repulsion!! ...
26.Meikle.Supernova_2002hh
... ejecta. Supernovae are suspected to be a major source of dust in the universe and the presence of new dust in SN 2002hh is expected to be observed at a later stage. This is only the second time for which a spectrum has been obtained of a supernova in 2.9-4.1 micron range (the other was SN 1987A whic ...
... ejecta. Supernovae are suspected to be a major source of dust in the universe and the presence of new dust in SN 2002hh is expected to be observed at a later stage. This is only the second time for which a spectrum has been obtained of a supernova in 2.9-4.1 micron range (the other was SN 1987A whic ...
mass loss of massive stars - of /proceedings
... bursts, large amounts of mass are ejected in the immediate surrounding. This deeply affects not only the star’s evolution, but also the structure of the interstellar medium, and thus the appearance of supernovae which occur in such environments. Mass loss is one of the main drivers of massive stars ...
... bursts, large amounts of mass are ejected in the immediate surrounding. This deeply affects not only the star’s evolution, but also the structure of the interstellar medium, and thus the appearance of supernovae which occur in such environments. Mass loss is one of the main drivers of massive stars ...
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.