Life Cycle of Stars
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a large poster that visually displays the four life cycles. 2) Use your notes, RQs, video notes and a computer or phone to complete the following: a) Name of star stage b) Color ...
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a large poster that visually displays the four life cycles. 2) Use your notes, RQs, video notes and a computer or phone to complete the following: a) Name of star stage b) Color ...
Document
... evolution - the timescale over which a star is evolves is too long for us to follow the evolution of any one star. Also, numerical modeling allows us to build up a picture of things that we cannot see (such as the core of a star). If the observations agree with the results predicted by the numerical ...
... evolution - the timescale over which a star is evolves is too long for us to follow the evolution of any one star. Also, numerical modeling allows us to build up a picture of things that we cannot see (such as the core of a star). If the observations agree with the results predicted by the numerical ...
Powerpoint Presentation (large file)
... – an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion begins ...
... – an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion begins ...
1) The following questions refer to the HR diagram
... C) As gravity overwhelms the electron degeneracy pressure, it will become a neutron star. D) As gravity overwhelms the electron degeneracy pressure, it will explode as a nova. E) It will cool down and become a cold black dwarf. 21) White dwarfs are so called because A) it amplifies the contrast with ...
... C) As gravity overwhelms the electron degeneracy pressure, it will become a neutron star. D) As gravity overwhelms the electron degeneracy pressure, it will explode as a nova. E) It will cool down and become a cold black dwarf. 21) White dwarfs are so called because A) it amplifies the contrast with ...
The Sun - Hicksville Public Schools
... weeks or months. During this short interval, a supernova can radiate as much energy as the Sun would emit over 10 billion years. The explosion expels much or all of a star's material at high velocity, driving a shock wave into the surrounding interstellar medium, where it sweeps up an expanding shel ...
... weeks or months. During this short interval, a supernova can radiate as much energy as the Sun would emit over 10 billion years. The explosion expels much or all of a star's material at high velocity, driving a shock wave into the surrounding interstellar medium, where it sweeps up an expanding shel ...
Lecture4
... The visible-light spectrum of the Sun is wrapped here end to end from red to blue. The dark “lines” are wavelengths that are absorbed by atoms in the Sun’s outer layers. There are millions of “lines” in the Sun’s spectrum. ...
... The visible-light spectrum of the Sun is wrapped here end to end from red to blue. The dark “lines” are wavelengths that are absorbed by atoms in the Sun’s outer layers. There are millions of “lines” in the Sun’s spectrum. ...
File
... where protons are added successively to produce the helium. This reaction is the starting point of zero-age main sequence stars Larger, hotter main sequence stars, operating at higher core temperatures, can fuse hydrogen via the CNO cycle where carbon, nitrogen and oxygen act as catalysts in the rea ...
... where protons are added successively to produce the helium. This reaction is the starting point of zero-age main sequence stars Larger, hotter main sequence stars, operating at higher core temperatures, can fuse hydrogen via the CNO cycle where carbon, nitrogen and oxygen act as catalysts in the rea ...
(a) Because the core of heavy-mass star never reaches high enough
... (a) apparent brightness and mass (b) apparent brightness and temperature (c) apparent brightness and distance (d) apparent brightness and pressure (e) apparent brightness and magnetic force Answer (c) 9. Where do stars form? (a) In cold, relatively dense molecular clouds (b) In binary systems where ...
... (a) apparent brightness and mass (b) apparent brightness and temperature (c) apparent brightness and distance (d) apparent brightness and pressure (e) apparent brightness and magnetic force Answer (c) 9. Where do stars form? (a) In cold, relatively dense molecular clouds (b) In binary systems where ...
KMS Universe Test Study Guide
... 2) What is a nebula? A cloud of gas and dust, from which stars are formed. 3) What force within a nebula helps the matter within the nebula coalesce? Gravity 4) Matter in nebulae forms into great spheres and starts to heat up and glow from heat and pressure. What is said to have been formed at this ...
... 2) What is a nebula? A cloud of gas and dust, from which stars are formed. 3) What force within a nebula helps the matter within the nebula coalesce? Gravity 4) Matter in nebulae forms into great spheres and starts to heat up and glow from heat and pressure. What is said to have been formed at this ...
Document
... • High mass-loss rates, and cool effective temperatures (~3000 K) • A dust shell hides most of the stellar luminosity and so the stars are seen only in the infrared. ...
... • High mass-loss rates, and cool effective temperatures (~3000 K) • A dust shell hides most of the stellar luminosity and so the stars are seen only in the infrared. ...
The Hertzsprung-Russell Diagram
... sequence K5 stars radiate the same amount of energy from each square meter. So, in order for the K5 giant to be more luminous, it must have more square meters; i.e, it must have a larger surface area, thus a larger radius. 5. The B0 I star is farthest away, as it is the most luminous among the star ...
... sequence K5 stars radiate the same amount of energy from each square meter. So, in order for the K5 giant to be more luminous, it must have more square meters; i.e, it must have a larger surface area, thus a larger radius. 5. The B0 I star is farthest away, as it is the most luminous among the star ...
(Star Stuff) ( 11-9-10)
... 3. High mass star (M > 4 solar masses) •Fusion of He,C,O,…..but not Fe (Iron) fusion Faster and faster Core collapses Supernova Produces all elements heavier than Fe and blows envelope apart ejecting to interstellar space most of its mass ...
... 3. High mass star (M > 4 solar masses) •Fusion of He,C,O,…..but not Fe (Iron) fusion Faster and faster Core collapses Supernova Produces all elements heavier than Fe and blows envelope apart ejecting to interstellar space most of its mass ...
Astronomy Assignment #1
... drive faster fusion rates and created higher luminosities. The higher luminosities “burn” mass faster and the star will then “burn” through its core reserves of hydrogen faster. Low mass stars have slower fusion rates because the fusion rate is slower due to the lower central pressure of these low m ...
... drive faster fusion rates and created higher luminosities. The higher luminosities “burn” mass faster and the star will then “burn” through its core reserves of hydrogen faster. Low mass stars have slower fusion rates because the fusion rate is slower due to the lower central pressure of these low m ...
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.