Stars Student Page Purpose To investigate stellar classification by
... upper left to the lower right portion of the diagram. This is on the Main Sequence portion of the diagram. 3. Even though stars in this portion of the diagram have relatively low surface temperatures, they have high luminosities because of their tremendous size. The stars in this portion of the grap ...
... upper left to the lower right portion of the diagram. This is on the Main Sequence portion of the diagram. 3. Even though stars in this portion of the diagram have relatively low surface temperatures, they have high luminosities because of their tremendous size. The stars in this portion of the grap ...
TAP 705-3: The parsec - Teaching Advanced Physics
... A unit of distance in common use amongst astronomers is the parsec. As the Earth moves in its orbit around the Sun, the position of nearby stars against the background of very distant stars seems to change. ...
... A unit of distance in common use amongst astronomers is the parsec. As the Earth moves in its orbit around the Sun, the position of nearby stars against the background of very distant stars seems to change. ...
Astrophysics Presentation
... Certain spectral lines appeared consistently at certain temperatures and disappeared at others Different lines appear with different degrees of ionisation – which results from different temperatures ...
... Certain spectral lines appeared consistently at certain temperatures and disappeared at others Different lines appear with different degrees of ionisation – which results from different temperatures ...
Astronomy Unit Period
... __________ 4. Which of the following statements is true about a star? a. A star’s outer layers are hot and thin. b. A star’s outer layers are hot and dense. c. A star’s inner layers are cool and dense. d. A star’s inner layers are hot and dense. __________ 5. Some of the light that radiates from a s ...
... __________ 4. Which of the following statements is true about a star? a. A star’s outer layers are hot and thin. b. A star’s outer layers are hot and dense. c. A star’s inner layers are cool and dense. d. A star’s inner layers are hot and dense. __________ 5. Some of the light that radiates from a s ...
16. Properties of Stars
... Lifetime on the Main Sequence How long will it be before MS stars run out of fuel? i.e. Hydrogen? How much fuel is there? M How fast is it consumed? L M How long before it is used up? Time = Amount/(rate it is being used) ...
... Lifetime on the Main Sequence How long will it be before MS stars run out of fuel? i.e. Hydrogen? How much fuel is there? M How fast is it consumed? L M How long before it is used up? Time = Amount/(rate it is being used) ...
Document
... • After the supernova explosion, a high mass star will become a neutron star. • After a supernova explosion, in a very high mass star the core that remains will be so massive, that without the energy created by nuclear fusion to support it, the core is swallowed by its own gravity. • The gravity of ...
... • After the supernova explosion, a high mass star will become a neutron star. • After a supernova explosion, in a very high mass star the core that remains will be so massive, that without the energy created by nuclear fusion to support it, the core is swallowed by its own gravity. • The gravity of ...
galaxies and stars - Valhalla High School
... magnitude is its brightness as seen from Earth • A star looks brighter the closer it is to Earth ...
... magnitude is its brightness as seen from Earth • A star looks brighter the closer it is to Earth ...
Branches of Earth Science Tools Used to Study Stars Constellations
... Shows the relationship between absolute brightness and surface temperature This is the single most important diagram that astronomers use ...
... Shows the relationship between absolute brightness and surface temperature This is the single most important diagram that astronomers use ...
Earth Space Systems Semester 1 Exam Astronomy Vocabulary Astronomical Unit-
... After the Variable stage of a Medium to Low Mass Star, the outer shell forms a Planetary Nebula around a hot, smaller and less luminous star called a White Dwarf. White Dwarfs are about the size of our Earth but still have a mass near the original Main Sequence star. Eventually the White Dwarf will ...
... After the Variable stage of a Medium to Low Mass Star, the outer shell forms a Planetary Nebula around a hot, smaller and less luminous star called a White Dwarf. White Dwarfs are about the size of our Earth but still have a mass near the original Main Sequence star. Eventually the White Dwarf will ...
Life Cycle of a Star - Intervention Worksheet
... The stages below are not in the right order. Number the stages in the correct order. _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a neb ...
... The stages below are not in the right order. Number the stages in the correct order. _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a neb ...
Why does the sky move?
... The first is because the Earth is spinning and second because the Earth itself is moving around the Sun. ...
... The first is because the Earth is spinning and second because the Earth itself is moving around the Sun. ...
Chapter 13
... Low luminosity; high temperature => White dwarfs are found in the lower left corner of the Hertzsprung-Russell diagram. ...
... Low luminosity; high temperature => White dwarfs are found in the lower left corner of the Hertzsprung-Russell diagram. ...
Black holes - Red Hook Central School District
... If Gravity wins over pressure, stellar corpse keeps collapsing without end, crushing itself out of existence Forming a Black Hole ...
... If Gravity wins over pressure, stellar corpse keeps collapsing without end, crushing itself out of existence Forming a Black Hole ...
Study Guide for 3RD Astronomy Exam
... List or identify the luminosity, mass, radius, temperature, and lifetime of an O main sequence star, the Sun and an M main sequence star. State the impact of convection in the envelope of very low mass stars on the stars main sequence lifetime. Describe or identify changes in a star during its main ...
... List or identify the luminosity, mass, radius, temperature, and lifetime of an O main sequence star, the Sun and an M main sequence star. State the impact of convection in the envelope of very low mass stars on the stars main sequence lifetime. Describe or identify changes in a star during its main ...
A-36_SF
... “Debris” disk? All the original small dust grains should have been blown from the system by the star. Any remaining dust must be from collisions of planetesimals! ...
... “Debris” disk? All the original small dust grains should have been blown from the system by the star. Any remaining dust must be from collisions of planetesimals! ...
GEARS Workshop Monday - Georgia Southern University
... Units/2-StellarEvolution/2Stars_7.html • Compare main sequence lifetimes, end states. ...
... Units/2-StellarEvolution/2Stars_7.html • Compare main sequence lifetimes, end states. ...
Dead Stars
... Radius vs. Mass for White Dwarfs (1) •Order of magnitude estimate for size of white dwarf R – Ignore factors of 2, , etc. •As we did before, assume a star of radius R and mass M •Divide the star in half – Each half has mass ½ M ~ M and are separated by a distance R ...
... Radius vs. Mass for White Dwarfs (1) •Order of magnitude estimate for size of white dwarf R – Ignore factors of 2, , etc. •As we did before, assume a star of radius R and mass M •Divide the star in half – Each half has mass ½ M ~ M and are separated by a distance R ...
Powerpoint - Physics and Astronomy
... c) in the cores of stars like the Sun. d) within planetary nebula e) They have always existed. Explanation: ...
... c) in the cores of stars like the Sun. d) within planetary nebula e) They have always existed. Explanation: ...
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.