Ay 1 – Final Exam
... 21. (2 points) Explain why the shape of the Milky Way Galaxy's rotation curve implies the presence of dark matter, given the distribution of visible matter in the Milky Way. What would the Galactic rotation curve look like if the majority of the matter were concentrated in the central regions of the ...
... 21. (2 points) Explain why the shape of the Milky Way Galaxy's rotation curve implies the presence of dark matter, given the distribution of visible matter in the Milky Way. What would the Galactic rotation curve look like if the majority of the matter were concentrated in the central regions of the ...
elementary measuring stars
... Absolute magnitude is defined as the brightness at which an object would appear if placed at a distance of 10 parsecs. As such, M is a measure of a star’s luminosity. Another magnitude used is colour index, the difference between a star’s brightness (in magnitudes) in different colour bands, usually ...
... Absolute magnitude is defined as the brightness at which an object would appear if placed at a distance of 10 parsecs. As such, M is a measure of a star’s luminosity. Another magnitude used is colour index, the difference between a star’s brightness (in magnitudes) in different colour bands, usually ...
answer key
... 4. In what state do stars spend most of their life cycle? (Our sun is currently in this phase) 5. What are the most common types of stars in our universe? 6. This type of star has a surface temperature of 45,000 degrees F and is up to 20 times the mass of the sun. 7. How long will our Sun live? ...
... 4. In what state do stars spend most of their life cycle? (Our sun is currently in this phase) 5. What are the most common types of stars in our universe? 6. This type of star has a surface temperature of 45,000 degrees F and is up to 20 times the mass of the sun. 7. How long will our Sun live? ...
Habitable Zones around Evolved Stars
... Factors determining the location of the habitable zone in evolved stars • L changes dramatically as a star evolves beyond the main sequence • ap is altered by changing M* or in extreme cases by tidal or gas drag • The albedoratio depends on planetary atmosphere, surface properties, => and the stell ...
... Factors determining the location of the habitable zone in evolved stars • L changes dramatically as a star evolves beyond the main sequence • ap is altered by changing M* or in extreme cases by tidal or gas drag • The albedoratio depends on planetary atmosphere, surface properties, => and the stell ...
Structure of the Sun
... 1) Enormous pressure and high temperatures of the sun’s core cause the atoms to separate into nuclei and electrons. 2) In the core (unlike on Earth), the energy and pressure strip electrons away from the atomic nuclei. 3) The nuclei have positive charges, so they tend to push away from each other. S ...
... 1) Enormous pressure and high temperatures of the sun’s core cause the atoms to separate into nuclei and electrons. 2) In the core (unlike on Earth), the energy and pressure strip electrons away from the atomic nuclei. 3) The nuclei have positive charges, so they tend to push away from each other. S ...
Fulltext PDF
... The process of formation of a star can be divided into three phases. The first, known as 'star formation', involves massive interstellar clouds or cloud fragments, which have cooled to the point where they are detectable in molecular lines (such as CO) but which are unable to collapse because of an ...
... The process of formation of a star can be divided into three phases. The first, known as 'star formation', involves massive interstellar clouds or cloud fragments, which have cooled to the point where they are detectable in molecular lines (such as CO) but which are unable to collapse because of an ...
ASTRONOMY - Frost Middle School
... • The center of the supernova (collapsed star) may contract into a very small but very dense ball of neutrons • This ball of neutrons is called Neutron Star • One teaspoon of matter from a neutron star would weigh 100 million metric tons of Earth • A lot of energy (100,000 suns) ...
... • The center of the supernova (collapsed star) may contract into a very small but very dense ball of neutrons • This ball of neutrons is called Neutron Star • One teaspoon of matter from a neutron star would weigh 100 million metric tons of Earth • A lot of energy (100,000 suns) ...
Goal: To understand how Saturn formed and what its core is
... • If the planet exerts the same force on the star as the star exerts on the planet, what will happen to the star (which is thousands to millions times more massive than the planet)? ...
... • If the planet exerts the same force on the star as the star exerts on the planet, what will happen to the star (which is thousands to millions times more massive than the planet)? ...
Stars on the HR Diagram
... plot of stars from the upper left to the lower right of the HR diagram, the “main sequence” and 90% of all stars plot along this curve. Comparing the physical aspects of a number of stars is much like an alien visiting Earth for 20 minutes and attempting to understand a human life cycle by observing ...
... plot of stars from the upper left to the lower right of the HR diagram, the “main sequence” and 90% of all stars plot along this curve. Comparing the physical aspects of a number of stars is much like an alien visiting Earth for 20 minutes and attempting to understand a human life cycle by observing ...
General Astronomy - Stockton University
... – Period: 1-300+days; Amplitude of variation: 7-16 mag. – These close binary systems consist of a main sequence, Sunlike star and a white dwarf. – They increase in brightness by 7 to 16 magnitudes in a matter of one to several hundred days. After the outburst, the star fades slowly to the initial br ...
... – Period: 1-300+days; Amplitude of variation: 7-16 mag. – These close binary systems consist of a main sequence, Sunlike star and a white dwarf. – They increase in brightness by 7 to 16 magnitudes in a matter of one to several hundred days. After the outburst, the star fades slowly to the initial br ...
Int. Sci. 9 - Universe Powerpoint
... • Used to estimate the sizes of stars & their distances, and to infer how stars change over time • Main Sequence Stars – about 90% of stars – The Sun lies in the middle of this band • Supergiants – less than 1%; very bright stars at the upper right of the diagram • White Dwarf – about 10% of stars; ...
... • Used to estimate the sizes of stars & their distances, and to infer how stars change over time • Main Sequence Stars – about 90% of stars – The Sun lies in the middle of this band • Supergiants – less than 1%; very bright stars at the upper right of the diagram • White Dwarf – about 10% of stars; ...
LIFE CYCLE OF STARS
... A Star’s Old Age to Death Medium Stars Cool at the end of the Red Giant stage faster than larger stars, so they begin to shed its gases outside its core forming a planetary nebula . The center of the small star then begins to cool to become a white dwarf and cools more to become a black dwarf. ...
... A Star’s Old Age to Death Medium Stars Cool at the end of the Red Giant stage faster than larger stars, so they begin to shed its gases outside its core forming a planetary nebula . The center of the small star then begins to cool to become a white dwarf and cools more to become a black dwarf. ...
Luminosity
... Main-sequence stars are fusing hydrogen into helium in their cores, like the Sun. Luminous mainsequence stars are hot (blue). Less luminous ones are cooler (yellow or red). ...
... Main-sequence stars are fusing hydrogen into helium in their cores, like the Sun. Luminous mainsequence stars are hot (blue). Less luminous ones are cooler (yellow or red). ...
Background Presentation
... The NASA E/PO Program at Sonoma State University A group of people working collaboratively to educate the public about current and future NASA high energy astrophysics/astronomy missions. Swift Led by Prof. Lynn Cominsky ...
... The NASA E/PO Program at Sonoma State University A group of people working collaboratively to educate the public about current and future NASA high energy astrophysics/astronomy missions. Swift Led by Prof. Lynn Cominsky ...
Charcteristic of Stars Powerpoint C
... approximately 695,000 km, or about 109 times the radius of Earth. So the sun would equal 1 solar radius. • In comparison white dwarfs are about the same size as Earth and would equal 0.01 solar radius. Supergiants can have sizes up to 1,000 solar radii. ...
... approximately 695,000 km, or about 109 times the radius of Earth. So the sun would equal 1 solar radius. • In comparison white dwarfs are about the same size as Earth and would equal 0.01 solar radius. Supergiants can have sizes up to 1,000 solar radii. ...
Name: Period:______ Date:______ Astronomy Vocabulary List
... Supernova- a massive explosion of a dying star. ...
... Supernova- a massive explosion of a dying star. ...
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.