MT 2 Answers Version C
... Measure the gravitational attraction between the mouse and a steel ball of known mass. ...
... Measure the gravitational attraction between the mouse and a steel ball of known mass. ...
An introduction to the HR diagram File
... radius and therefore are very luminous ( therefore have high absolute magnitude). However they are much cooler than would be expected for stars of large radius. White dwarf stars White dwarfs are high temperature stars but their small radius (some around the size of Earth) is abnormal for such high ...
... radius and therefore are very luminous ( therefore have high absolute magnitude). However they are much cooler than would be expected for stars of large radius. White dwarf stars White dwarfs are high temperature stars but their small radius (some around the size of Earth) is abnormal for such high ...
d 2
... • Some have names that go back to ancient times (e.g. Castor and Pollux, Greek mythology) • Some were named by Arab astronomers (e.g. Aldebaran, Algol, etc.) • Since the 17th century we use a scheme that lists stars by constellation – in order of their apparent brightness – labeled alphabetically in ...
... • Some have names that go back to ancient times (e.g. Castor and Pollux, Greek mythology) • Some were named by Arab astronomers (e.g. Aldebaran, Algol, etc.) • Since the 17th century we use a scheme that lists stars by constellation – in order of their apparent brightness – labeled alphabetically in ...
Astronomy Library wk 7.cwk (WP)
... At different points in a stars life, it is different processes which hold a star up against gravity. In following a star’s evolution we will follow its path in the H-R Diagram (how its temperature and luminosity vary). ...
... At different points in a stars life, it is different processes which hold a star up against gravity. In following a star’s evolution we will follow its path in the H-R Diagram (how its temperature and luminosity vary). ...
test - Scioly.org
... 16. Expressed in solar masses, a type 1a supernova will occur when the left hand star reaches what mass? 17. Expressed in kg, and in scientific notation, a type 1a supernova will occur when the left hand star reaches what mass? 18. This point at which a type 1a supernova occurs is named after and In ...
... 16. Expressed in solar masses, a type 1a supernova will occur when the left hand star reaches what mass? 17. Expressed in kg, and in scientific notation, a type 1a supernova will occur when the left hand star reaches what mass? 18. This point at which a type 1a supernova occurs is named after and In ...
powerpoint - Physics @ IUPUI
... • Remember that most stars are in binary systems! • At the end of the life of the biggest star, sometimes the other stars get away because the dying star looses a lot of mass. ...
... • Remember that most stars are in binary systems! • At the end of the life of the biggest star, sometimes the other stars get away because the dying star looses a lot of mass. ...
09astrophysics_2007Nov
... If we can measure the color of a star, we can calculate its temperature (Wien’s Law) Measure magnitude of star through color filters Color Index=C.I. = B-V is measure of temperature of star. ...
... If we can measure the color of a star, we can calculate its temperature (Wien’s Law) Measure magnitude of star through color filters Color Index=C.I. = B-V is measure of temperature of star. ...
doc
... becomes even bigger and more luminous. This 2nd ascent of the red giant branch “asymptotic giant branch (AGB)”. Now the carbon (He ashes) core becomes degenerate before C can ignite (if original mass of star is less than about 8 Mo), and the temperature stops increasing no more nuclear burning p ...
... becomes even bigger and more luminous. This 2nd ascent of the red giant branch “asymptotic giant branch (AGB)”. Now the carbon (He ashes) core becomes degenerate before C can ignite (if original mass of star is less than about 8 Mo), and the temperature stops increasing no more nuclear burning p ...
Life of a star - bahringcarthnoians
... times the mass of our sun. They have a large radius (up to hundreds of times larger than our sun) and their surface temperature is 5,000° Kelvin and lower. They are yelloworange to red in colour. Red giants have burnt up all the hydrogen fuel in their cores. When this happens, nuclear reactions stop ...
... times the mass of our sun. They have a large radius (up to hundreds of times larger than our sun) and their surface temperature is 5,000° Kelvin and lower. They are yelloworange to red in colour. Red giants have burnt up all the hydrogen fuel in their cores. When this happens, nuclear reactions stop ...
(a) Because the core of heavy-mass star never reaches high enough
... 7. Which of the following is the right description of the main sequence stars? (a) Stars on the main sequence are all fusing hydrogen into helium in their cores. (b) Stars on the main sequence are all fusing helium into carbon in their cores. (c) Stars on the main sequence are all fusing carbon int ...
... 7. Which of the following is the right description of the main sequence stars? (a) Stars on the main sequence are all fusing hydrogen into helium in their cores. (b) Stars on the main sequence are all fusing helium into carbon in their cores. (c) Stars on the main sequence are all fusing carbon int ...
HR Diagram - Geneva 304
... 51. Compare and contrast stellar Population I with stellar Population II. Do the stars in the galactic cluster Pleiades belong to stellar Population I or II? ...
... 51. Compare and contrast stellar Population I with stellar Population II. Do the stars in the galactic cluster Pleiades belong to stellar Population I or II? ...
Evolution Cycle of Stars
... • These stars are composed mainly of neutrons and are produced when a supernova explodes, forcing the protons and electrons to combine to produce a neutron star. • Neutron stars are very dense. Typical stars having a mass of three times the Sun but a diameter of only 20 km. If its mass is any greate ...
... • These stars are composed mainly of neutrons and are produced when a supernova explodes, forcing the protons and electrons to combine to produce a neutron star. • Neutron stars are very dense. Typical stars having a mass of three times the Sun but a diameter of only 20 km. If its mass is any greate ...
Document
... There are particular wavelengths that are missing The missing wavelengths correspond to the absorption spectrum of a number of elements Although is seems sensible to assume that the elements concerned are in the Earth’s atmosphere, this assumption is incorrect Wavelengths would still be abse ...
... There are particular wavelengths that are missing The missing wavelengths correspond to the absorption spectrum of a number of elements Although is seems sensible to assume that the elements concerned are in the Earth’s atmosphere, this assumption is incorrect Wavelengths would still be abse ...
Life Cycle of a Star notes
... We now know that stars move through a complex life cycle – they are created, live extremely long lives and then expire. By studying different stars in various stages of development, astronomers have now established a detailed process for their life cycle. ...
... We now know that stars move through a complex life cycle – they are created, live extremely long lives and then expire. By studying different stars in various stages of development, astronomers have now established a detailed process for their life cycle. ...
Evolution of Stars and Galaxies
... If supernova core is 3 or more times as massive as Sun core will collapse Not even light can escape An event horizon anything crossing this will go (region nothing can escape) Other stars orbit around it as usual ...
... If supernova core is 3 or more times as massive as Sun core will collapse Not even light can escape An event horizon anything crossing this will go (region nothing can escape) Other stars orbit around it as usual ...
Stellar Physics - University of Reading
... Classical Mechanics and Optics Thermodynamics and Statistical Mechanics Atomic and Molecular Physics Ideas from Observational Astronomy ...
... Classical Mechanics and Optics Thermodynamics and Statistical Mechanics Atomic and Molecular Physics Ideas from Observational Astronomy ...
formation2
... stars orbit around the galaxy moving in and out of spiral arms • From the HR diagram, by far the most luminous stars are the O-type stars. Their luminosity can be 100,000 times the Sun’s. • Why is the spiral structure in galaxies so ...
... stars orbit around the galaxy moving in and out of spiral arms • From the HR diagram, by far the most luminous stars are the O-type stars. Their luminosity can be 100,000 times the Sun’s. • Why is the spiral structure in galaxies so ...
Stars - MrCrabtreesScience
... If remaining core is >3 times the mass of the sun it forms a Black Hole • All the matter is squeezed into a space smaller ...
... If remaining core is >3 times the mass of the sun it forms a Black Hole • All the matter is squeezed into a space smaller ...
Star
A star is a luminous sphere of plasma held together by its own gravity. The nearest star to Earth is the Sun. Other stars are visible from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth. Historically, the most prominent stars were grouped into constellations and asterisms, and the brightest stars gained proper names. Extensive catalogues of stars have been assembled by astronomers, which provide standardized star designations.For at least a portion of its life, a star shines due to thermonuclear fusion of hydrogen into helium in its core, releasing energy that traverses the star's interior and then radiates into outer space. Once the hydrogen in the core of a star is nearly exhausted, almost all naturally occurring elements heavier than helium are created by stellar nucleosynthesis during the star's lifetime and, for some stars, by supernova nucleosynthesis when it explodes. Near the end of its life, a star can also contain degenerate matter. Astronomers can determine the mass, age, metallicity (chemical composition), and many other properties of a star by observing its motion through space, luminosity, and spectrum respectively. The total mass of a star is the principal determinant of its evolution and eventual fate. Other characteristics of a star, including diameter and temperature, change over its life, while the star's environment affects its rotation and movement. A plot of the temperature of many stars against their luminosities, known as a Hertzsprung–Russell diagram (H–R diagram), allows the age and evolutionary state of a star to be determined.A star's life begins with the gravitational collapse of a gaseous nebula of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. Once the stellar core is sufficiently dense, hydrogen becomes steadily converted into helium through nuclear fusion, releasing energy in the process. The remainder of the star's interior carries energy away from the core through a combination of radiative and convective processes. The star's internal pressure prevents it from collapsing further under its own gravity. Once the hydrogen fuel at the core is exhausted, a star with at least 0.4 times the mass of the Sun expands to become a red giant, in some cases fusing heavier elements at the core or in shells around the core. The star then evolves into a degenerate form, recycling a portion of its matter into the interstellar environment, where it will contribute to the formation of a new generation of stars with a higher proportion of heavy elements. Meanwhile, the core becomes a stellar remnant: a white dwarf, a neutron star, or (if it is sufficiently massive) a black hole.Binary and multi-star systems consist of two or more stars that are gravitationally bound, and generally move around each other in stable orbits. When two such stars have a relatively close orbit, their gravitational interaction can have a significant impact on their evolution. Stars can form part of a much larger gravitationally bound structure, such as a star cluster or a galaxy.