Stars: Other Suns
... • Measure directly only with binary systems of stars (lots!) • Revolve around center of mass • Apply Kepler’s 3rd law to get sum of masses from orbital period, separation (need distance!) ...
... • Measure directly only with binary systems of stars (lots!) • Revolve around center of mass • Apply Kepler’s 3rd law to get sum of masses from orbital period, separation (need distance!) ...
Sun, Star Types and Luminosity
... band of stars on the star diagram. b. Energy comes from nuclear fusion as they convert Hydrogen to Helium. c. The sun is a typical Main Sequence star. d. Most stars (about 90%) are Main Sequence Stars. e. For these stars, the hotter, the brighter ...
... band of stars on the star diagram. b. Energy comes from nuclear fusion as they convert Hydrogen to Helium. c. The sun is a typical Main Sequence star. d. Most stars (about 90%) are Main Sequence Stars. e. For these stars, the hotter, the brighter ...
Document
... Would the surface temperature of white dwarf stars be higher or lower than red supergiants? (Circle one of the bold words) ...
... Would the surface temperature of white dwarf stars be higher or lower than red supergiants? (Circle one of the bold words) ...
TU Muscae and the Early-type Overcontact Binaries
... Binary orbital plane is oriented so that the two stars pass in front of one another as seen from Earth. The light curve is rich in information about the two stars. ...
... Binary orbital plane is oriented so that the two stars pass in front of one another as seen from Earth. The light curve is rich in information about the two stars. ...
Astronomy Learning Objectives and Study Questions for Chapter 12
... 7. Star clusters are important for understanding stellar evolution because the stars in them are similar in most respects, except _____. A. ages B. distances from Earth C. masses D. initial compositions E. they are similar in all these respects 8. Which of the star clusters plotted on the accompanyi ...
... 7. Star clusters are important for understanding stellar evolution because the stars in them are similar in most respects, except _____. A. ages B. distances from Earth C. masses D. initial compositions E. they are similar in all these respects 8. Which of the star clusters plotted on the accompanyi ...
Characteristics of Stars
... • The scientific name for the twinkling of stars is stellar scintillation • Stars twinkle when we see them from the Earth's surface because we are viewing them through thick layers of turbulent (moving) air in the Earth's atmosphere. ...
... • The scientific name for the twinkling of stars is stellar scintillation • Stars twinkle when we see them from the Earth's surface because we are viewing them through thick layers of turbulent (moving) air in the Earth's atmosphere. ...
20.1 Notes
... This huge, bright explosion is called a Type II _________________________. If the core that remains after a supernova has a mass of 1.4 – 3 solar masses it becomes a _______________ star, a very dense star that is a source of pulsating radio waves called _____________. ...
... This huge, bright explosion is called a Type II _________________________. If the core that remains after a supernova has a mass of 1.4 – 3 solar masses it becomes a _______________ star, a very dense star that is a source of pulsating radio waves called _____________. ...
STARS
... Nuclear fusion gives the star enough electromagnetic energy to begin shining and a star is born ...
... Nuclear fusion gives the star enough electromagnetic energy to begin shining and a star is born ...
Ch. 27 Stars & Galaxies
... • Constellations: Star groups that shift in fixed patterns as viewed from Earth ...
... • Constellations: Star groups that shift in fixed patterns as viewed from Earth ...
File
... core heats up and ________ begins to fuse into other elements (carbon) outer surface expands up to _____ times huge size mean low temperature... it is now a ______ ________. The outer layer of gas gets blown off producing a cloud of gas called a ___________ ______________ leaving a hot, de ...
... core heats up and ________ begins to fuse into other elements (carbon) outer surface expands up to _____ times huge size mean low temperature... it is now a ______ ________. The outer layer of gas gets blown off producing a cloud of gas called a ___________ ______________ leaving a hot, de ...
The Lives of Stars
... than large-mass stars, so they have much longer lives • stars that have less mass than the sun use their fuel slowly, and can live for up to 200 billion years • medium-mass stars like the sun live for about 10 billion years • astronomers think the sun is about 4.6 billion years old, so it is almost ...
... than large-mass stars, so they have much longer lives • stars that have less mass than the sun use their fuel slowly, and can live for up to 200 billion years • medium-mass stars like the sun live for about 10 billion years • astronomers think the sun is about 4.6 billion years old, so it is almost ...
main sequence star
... • Small mass stars will collapse into white dwarfs after being red giants. • The outer gases are lost, which allows us to see the core of the star. The white dwarf is very dense and hot. The emit (release) less light than they did when they were stars. • As these white dwarfs cool they become fainte ...
... • Small mass stars will collapse into white dwarfs after being red giants. • The outer gases are lost, which allows us to see the core of the star. The white dwarf is very dense and hot. The emit (release) less light than they did when they were stars. • As these white dwarfs cool they become fainte ...
The Stars
... The Stars Stars vary greatly in size, brightness, temperature, and colour. Here are some of the things we have learned about the properties of stars. Measuring distance Just as with the kilometre, the AU is not very useful when we start to study stuff outside of our Solar System. A much larger unit ...
... The Stars Stars vary greatly in size, brightness, temperature, and colour. Here are some of the things we have learned about the properties of stars. Measuring distance Just as with the kilometre, the AU is not very useful when we start to study stuff outside of our Solar System. A much larger unit ...
Life Cycle of a Star
... Neutron Star a star that has collapsed to a point at which all particles are neutrons A neutron star that spins and sends out beams of radiation is called a pulsar ...
... Neutron Star a star that has collapsed to a point at which all particles are neutrons A neutron star that spins and sends out beams of radiation is called a pulsar ...
Problem set 1 1. The binding energy per nucleon for 56Fe is 8.8MeV
... 1. The binding energy per nucleon for 56 Fe is 8.8 MeV per nucleon. Estimate the total energy released per kilogram of matter by the sequence of reactions which fuse hydrogen to iron. 2. The main sequence of the Pleiades cluster of stars consists of stars with mass less than 6M ; the more massive s ...
... 1. The binding energy per nucleon for 56 Fe is 8.8 MeV per nucleon. Estimate the total energy released per kilogram of matter by the sequence of reactions which fuse hydrogen to iron. 2. The main sequence of the Pleiades cluster of stars consists of stars with mass less than 6M ; the more massive s ...
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.