Big Bang and Life Cycle of Stars
... - Leaving the dying star surrounded by gas clouds - Due to continual pressure on the core, these stars will become white dwarfs – which can be about the same size as the earth, but with the mass of a star. - Where do they move to on the HR diagram at this point? ...
... - Leaving the dying star surrounded by gas clouds - Due to continual pressure on the core, these stars will become white dwarfs – which can be about the same size as the earth, but with the mass of a star. - Where do they move to on the HR diagram at this point? ...
Stellar Evolution – Life of a Star
... EQUILIBRIUM. The liberation of energy from the interior of the star is balanced by the energy released at the surface of the star. The energy is produced by hydrogen burning in the core of star (conversion by fusion of H to He). • A second property is HYDROSTATIC EQUILIBRIUM. There is sufficient pre ...
... EQUILIBRIUM. The liberation of energy from the interior of the star is balanced by the energy released at the surface of the star. The energy is produced by hydrogen burning in the core of star (conversion by fusion of H to He). • A second property is HYDROSTATIC EQUILIBRIUM. There is sufficient pre ...
Name Date Life and Death of a Star 2015 1. In the main
... A. the mass of the star is slowly increasing B. hydrogen fusing to helium makes the core more dense C. carbon and iron are accumulating in the core In a timeline that shows the sequence of events that occurs during the formation of a star, what happens after the temperature increases in a proto-star ...
... A. the mass of the star is slowly increasing B. hydrogen fusing to helium makes the core more dense C. carbon and iron are accumulating in the core In a timeline that shows the sequence of events that occurs during the formation of a star, what happens after the temperature increases in a proto-star ...
Main-sequence stage Stellar lifetimes
... – Low-mass stars: the RR Lyrae variables are white horizontalbranch stars – Type II Cepheids are also low-mass stars. ...
... – Low-mass stars: the RR Lyrae variables are white horizontalbranch stars – Type II Cepheids are also low-mass stars. ...
Homework Problems for Quiz 1 – AY 5 – Spring 2013
... 11. Star A has twice the trigonometric parallax angle and twice the luminosity of Star B. (Assume no dust toward either star) a) What are the relative distances of the two stars? ...
... 11. Star A has twice the trigonometric parallax angle and twice the luminosity of Star B. (Assume no dust toward either star) a) What are the relative distances of the two stars? ...
E2 Stellar radiation and stellar types
... • The point of classifying the various types of stars is to see is any patterns exists. A useful way of making the comparison is the H-R diagram. Each dot on the diagram represents a different star. • The vertical axis is the luminosity of the star. It should be noted that the scale is not a linear ...
... • The point of classifying the various types of stars is to see is any patterns exists. A useful way of making the comparison is the H-R diagram. Each dot on the diagram represents a different star. • The vertical axis is the luminosity of the star. It should be noted that the scale is not a linear ...
The Birth of Stars Guiding Questions • Because stars shine by
... causes it to heat and begin glowing ...
... causes it to heat and begin glowing ...
The Galactic Super Star Cluster Westerlund 1
... times the mass of Orion. Therefore, we would have expected diffuse emission with L x = 3x10 35 erg s-1, which is five times more flux than we observe. We suggest that the IMF is nonstandard, as is often claimed for young, massive star clusters. ...
... times the mass of Orion. Therefore, we would have expected diffuse emission with L x = 3x10 35 erg s-1, which is five times more flux than we observe. We suggest that the IMF is nonstandard, as is often claimed for young, massive star clusters. ...
File
... per second, how long would it take to reach Proxima Centauri, the nearest star to Earth other than our Sun? Proxima Centauri is 4.01 ´ 1013 kilometers from Earth. Hint: there are ...
... per second, how long would it take to reach Proxima Centauri, the nearest star to Earth other than our Sun? Proxima Centauri is 4.01 ´ 1013 kilometers from Earth. Hint: there are ...
Brock physics - Brock University
... (a) Fusion of two 3 He nuclei into a 4 He nucleus. (b) Fusion of hydrogen and deuterium into 3 He. (c) Fusion of two protons into deuterium with a release of a positron, a neutrino and energy. (d) [None of the above.] 38. When four hydrogen nuclei fuse to form a helium nucleus, the total mass at the ...
... (a) Fusion of two 3 He nuclei into a 4 He nucleus. (b) Fusion of hydrogen and deuterium into 3 He. (c) Fusion of two protons into deuterium with a release of a positron, a neutrino and energy. (d) [None of the above.] 38. When four hydrogen nuclei fuse to form a helium nucleus, the total mass at the ...
Stars
... Each second, the Sun produces 4 × 1026 joules of energy. It would take 2,000 million nuclear power plants a whole year to produce the same amount of energy on Earth. In the Sun, and in most stars, hydrogen atoms fuse together to form helium. This provides the energy for life on Earth. 3 of 19 ...
... Each second, the Sun produces 4 × 1026 joules of energy. It would take 2,000 million nuclear power plants a whole year to produce the same amount of energy on Earth. In the Sun, and in most stars, hydrogen atoms fuse together to form helium. This provides the energy for life on Earth. 3 of 19 ...
Final Exam Review (Word doc)
... is caused by a) the density of the gas in the stellar atmosphere. b) the energy-level structure of the atom. c) the temperature of the stellar atmosphere. d) the Doppler shift. 29. A full moon can never rise at midnight. 30. From Earth, Mercury is difficult to see mostly because it always appears ne ...
... is caused by a) the density of the gas in the stellar atmosphere. b) the energy-level structure of the atom. c) the temperature of the stellar atmosphere. d) the Doppler shift. 29. A full moon can never rise at midnight. 30. From Earth, Mercury is difficult to see mostly because it always appears ne ...
chapter 28 pages 747-752
... • This is the longest stage of a stars life. • 4. In medium sized stars, once all H has been fused into He, He then starts to fuse into C during the Red Giant stage ...
... • This is the longest stage of a stars life. • 4. In medium sized stars, once all H has been fused into He, He then starts to fuse into C during the Red Giant stage ...
Earth Science 25.2A : Stellar Evolution
... As the star expands, it’s surface cools, which explains the star’s reddish appearance. During expansion, the core continues to collapse and heat until it reaches 100 million K. ...
... As the star expands, it’s surface cools, which explains the star’s reddish appearance. During expansion, the core continues to collapse and heat until it reaches 100 million K. ...
HERE - physicsisphun.org
... • Cooler objects glow with light intensity at the longer wavelengths or more toward the red end of the spectrum. Spectral Lines and composition ...
... • Cooler objects glow with light intensity at the longer wavelengths or more toward the red end of the spectrum. Spectral Lines and composition ...
Powerpoint of lecture 1
... would have at 10 pc. If D = distance of star: M = m – 5 log10(D/10pc). [We can hence also define the distance modulus m-M by: m - M = 5 log10(D/10pc).] ...
... would have at 10 pc. If D = distance of star: M = m – 5 log10(D/10pc). [We can hence also define the distance modulus m-M by: m - M = 5 log10(D/10pc).] ...
Astro 1 & 100 Levine Homework Stars Name:____________________________
... Part I — Properties of Stars You may want to do the lecture-tutorial on pg 33, Apparent and Absolute Magnitude of Stars, prior to doing this portion of the homework, if you need a refresher on m and M. Ranking questions are 2 points each. Consider the following table of stars: ...
... Part I — Properties of Stars You may want to do the lecture-tutorial on pg 33, Apparent and Absolute Magnitude of Stars, prior to doing this portion of the homework, if you need a refresher on m and M. Ranking questions are 2 points each. Consider the following table of stars: ...
Life cycle of low mass stars
... release as heavier elements are fused, the outer layer grow tremendously. ...
... release as heavier elements are fused, the outer layer grow tremendously. ...
ref H-R Spectral types
... Mass and luminosity If you’ve got a line like this, then you can predict luminosity from mass, and vice versa ...
... Mass and luminosity If you’ve got a line like this, then you can predict luminosity from mass, and vice versa ...
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.