Astronomy 12 - hrsbstaff.ednet.ns.ca
... hydrogen, and that the Sun's current mass was its mass before main-sequence burning. You will use some known properties of the Sun, and the knowledge that the Sun fuses hydrogen into helium. (i) From the internet, find the mass (in kg) and luminosity (in Watts) of the Sun. (ii) The Sun's principal r ...
... hydrogen, and that the Sun's current mass was its mass before main-sequence burning. You will use some known properties of the Sun, and the knowledge that the Sun fuses hydrogen into helium. (i) From the internet, find the mass (in kg) and luminosity (in Watts) of the Sun. (ii) The Sun's principal r ...
Post-Main Sequence Evolution – Low and Intermediate Mass Stars
... deposited by the outgoing light in the atoms near the star’s surface that absorb it. In red giants, grains may also form and be pushed out by the light. ...
... deposited by the outgoing light in the atoms near the star’s surface that absorb it. In red giants, grains may also form and be pushed out by the light. ...
1st EXAM VERSION C - Department of Physics and Astronomy
... A. *It is not possible to measure the star's mass accurately. B. There are several ways to measure its mass accurately. C. Its mass can be measured accurately only if its luminosity and temperature can be measured. D. Its mass can be measured accurately only if its distance can be found. 42. A refle ...
... A. *It is not possible to measure the star's mass accurately. B. There are several ways to measure its mass accurately. C. Its mass can be measured accurately only if its luminosity and temperature can be measured. D. Its mass can be measured accurately only if its distance can be found. 42. A refle ...
here - Tenafly Middle School
... Russell observed that stars with higher temperatures also have brighter absolute magnitudes. • They developed a graph to show this relationship (i.e. the Hertzsprung-Russel Diagram; H-R Diagram). • They placed temperatures across the bottom and absolute magnitudes up one side, showing the relationsh ...
... Russell observed that stars with higher temperatures also have brighter absolute magnitudes. • They developed a graph to show this relationship (i.e. the Hertzsprung-Russel Diagram; H-R Diagram). • They placed temperatures across the bottom and absolute magnitudes up one side, showing the relationsh ...
SAMPLE TEST: Stars and Galaxies Multiple Choice Identify the letter
... ____ 21. A star is said to be born when ____. a. a protostar reaches a temperature high enough for nuclear fusion to begin b. a red giant collapses on itself and becomes a black hole c. pressure within a protostar becomes so great that a supernova occurs d. a dark, cool interstellar cloud begins to ...
... ____ 21. A star is said to be born when ____. a. a protostar reaches a temperature high enough for nuclear fusion to begin b. a red giant collapses on itself and becomes a black hole c. pressure within a protostar becomes so great that a supernova occurs d. a dark, cool interstellar cloud begins to ...
Stellar Characteristics and Evolution
... helium-burning shell is not very stable - this causes the star to pulsate in both size and luminosity. As time goes on these pulsations get more and more severe (stars in this stage are sometimes known as the “Mira Giants”), becoming so great that the star actually starts to shed significant amounts ...
... helium-burning shell is not very stable - this causes the star to pulsate in both size and luminosity. As time goes on these pulsations get more and more severe (stars in this stage are sometimes known as the “Mira Giants”), becoming so great that the star actually starts to shed significant amounts ...
stars
... which is well understood to originate from a flattened circumstellar disk (e.g. Struve, 1931), can come and go episodically on time scales of days to decades. ...
... which is well understood to originate from a flattened circumstellar disk (e.g. Struve, 1931), can come and go episodically on time scales of days to decades. ...
Characteristics of Stars
... Stars that glow blue-white are the hottest (15,000 degrees Celsius) Rigel ...
... Stars that glow blue-white are the hottest (15,000 degrees Celsius) Rigel ...
“Reach for the Stars” Practice Exam
... Part II: Type Ia Supernova Background information: A Type I supernova event may occur within binary system having a white dwarf and a red giant in relatively close proximity. The exceedingly strong gravitational attraction of the white dwarf attracts materials from the outer layers of its red giant ...
... Part II: Type Ia Supernova Background information: A Type I supernova event may occur within binary system having a white dwarf and a red giant in relatively close proximity. The exceedingly strong gravitational attraction of the white dwarf attracts materials from the outer layers of its red giant ...
Stars
... that is the beginning of a star (PLANETS are also formed this way) • Dwarf: a main sequence star or, the smallest of stars (up to 20 times larger than our sun and up to 20,000 times brighter. Our sun is a dwarf star.) ...
... that is the beginning of a star (PLANETS are also formed this way) • Dwarf: a main sequence star or, the smallest of stars (up to 20 times larger than our sun and up to 20,000 times brighter. Our sun is a dwarf star.) ...
HW11
... temperature. So they are on the right side of the diagram. But their luminosity is huge. This is because their radius is gigantic. 4) Understand spectral typing. Why the hydrogen lines become large as the surface temperature increases until they reach spectral type A. Then as the temperature increas ...
... temperature. So they are on the right side of the diagram. But their luminosity is huge. This is because their radius is gigantic. 4) Understand spectral typing. Why the hydrogen lines become large as the surface temperature increases until they reach spectral type A. Then as the temperature increas ...
Chapter12 (with interactive links)
... After helium is used up in the core, hydrogen and helium fusion continues in shells around non-fusing carbon core. Outer layers expand and cool => asymptotic giant branch of the H-R diagram. ...
... After helium is used up in the core, hydrogen and helium fusion continues in shells around non-fusing carbon core. Outer layers expand and cool => asymptotic giant branch of the H-R diagram. ...
Sun - TeacherWeb
... http://scifiles.larc.nasa.gov/text/kids/Problem_Board/problems/sound/sound_waves2.html ...
... http://scifiles.larc.nasa.gov/text/kids/Problem_Board/problems/sound/sound_waves2.html ...
Our Universe
... the energy and matter that exists in the universe today. •The Big Bang occurred 13.8-15 Billion years ago. •Hydrogen and Helium, the makeup of stars, were the first two elements formed in less than a quarter of a second! •The explosion was so enormous, that all objects in the universe are still movi ...
... the energy and matter that exists in the universe today. •The Big Bang occurred 13.8-15 Billion years ago. •Hydrogen and Helium, the makeup of stars, were the first two elements formed in less than a quarter of a second! •The explosion was so enormous, that all objects in the universe are still movi ...
Life Cycle of a Star - Intervention Worksheet
... After a low or medium mass or star becomes a red giant, the outer parts grow bigger and drift into space, forming a cloud of gas called a planetary nebula. The blue-white hot core of the star that is left behind cools and becomes a white dwarf. The white dwarf eventually runs out of fuel and dies as ...
... After a low or medium mass or star becomes a red giant, the outer parts grow bigger and drift into space, forming a cloud of gas called a planetary nebula. The blue-white hot core of the star that is left behind cools and becomes a white dwarf. The white dwarf eventually runs out of fuel and dies as ...
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.