HERE
... a shock wave from the heat outward, expanding the outer layers of the star. The temperature and pressure conditions in the core increase enough to induce the fusion of heavier elements late in its life. Betelgeuse, pictured at left, is a red supergiant. It is nearing the end of its life and will soo ...
... a shock wave from the heat outward, expanding the outer layers of the star. The temperature and pressure conditions in the core increase enough to induce the fusion of heavier elements late in its life. Betelgeuse, pictured at left, is a red supergiant. It is nearing the end of its life and will soo ...
Sample final exam
... moving or if the other galaxy is moving. Hint: M31 contains more stars than the Milky Way, and the Milky Way contains more stars than the LMC. 20. Population I stars are those that lie on the disc portion of a galaxy; population II stars are those that exist in the bulge of a galaxy (text, page 159) ...
... moving or if the other galaxy is moving. Hint: M31 contains more stars than the Milky Way, and the Milky Way contains more stars than the LMC. 20. Population I stars are those that lie on the disc portion of a galaxy; population II stars are those that exist in the bulge of a galaxy (text, page 159) ...
Study Guide: Chapters 32-‐34 FROSH CHAPTER 32 1. What is
... 18. A star somewhat larger than our Sun produces more heat as it contracts. This star will then fuse _____ into heavier elements. ...
... 18. A star somewhat larger than our Sun produces more heat as it contracts. This star will then fuse _____ into heavier elements. ...
Presentation for perspective graduate students 2006
... not too hot and not too cold, many hydrogen atoms have their electron in the n = 2 orbit: hence strong absorption ...
... not too hot and not too cold, many hydrogen atoms have their electron in the n = 2 orbit: hence strong absorption ...
powerpoints - Georgia Southern University Astrophysics
... Would elements heavier than carbon exist? a. Yes, all stars create heavier elements than carbon when they become a supernova. b. Yes, but there would be far fewer heavier elements because high-mass stars form elements like iron far more prolifically than low-mass stars. c. No, the core temperatures ...
... Would elements heavier than carbon exist? a. Yes, all stars create heavier elements than carbon when they become a supernova. b. Yes, but there would be far fewer heavier elements because high-mass stars form elements like iron far more prolifically than low-mass stars. c. No, the core temperatures ...
Life Cycle of a Star - Intervention Worksheet
... The stages below are not in the right order. Number the stages in the correct order. _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a neb ...
... The stages below are not in the right order. Number the stages in the correct order. _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a neb ...
Stars Life Cycle WS
... The stages below are not in the right order. Number the stages in the correct order. _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a neb ...
... The stages below are not in the right order. Number the stages in the correct order. _____ The star begins to run out of fuel and expands into a red giant or red super giant. _____ Stars start out as diffused clouds of gas and dust drifting through space. A single one of these clouds is called a neb ...
astronomy practice Answers - hhs-snc1d
... d) gravity and outward pressure. (gravity and nuclear fusion) 12) Our Sun is about _________ years old and about _________ through its life span. a) 5 billion years, half b) 12 billion years, third c) 5 million years, third d) 10 billion years, 90 percent 13) When the sun runs out of Hydrogen and st ...
... d) gravity and outward pressure. (gravity and nuclear fusion) 12) Our Sun is about _________ years old and about _________ through its life span. a) 5 billion years, half b) 12 billion years, third c) 5 million years, third d) 10 billion years, 90 percent 13) When the sun runs out of Hydrogen and st ...
Astronomy 1 – Winter 2011
... not too hot and not too cold, many hydrogen atoms have their electron in the n = 2 orbit: hence strong absorption ...
... not too hot and not too cold, many hydrogen atoms have their electron in the n = 2 orbit: hence strong absorption ...
Sammy Nagel · Annie Jump Cannon
... She classified over 350000 stars.1.She also classified over 300 rare types of stars.2.Annie organized and collected photos for Harvard.3.She added over 300000 photos to their collection.4.Harvard had 200000 photos before Annie came, and 500000 photos after she left.5.She got an award named after her ...
... She classified over 350000 stars.1.She also classified over 300 rare types of stars.2.Annie organized and collected photos for Harvard.3.She added over 300000 photos to their collection.4.Harvard had 200000 photos before Annie came, and 500000 photos after she left.5.She got an award named after her ...
HW 5 Solutions What are “black smokers?” Where in our solar
... Figure 11.10: NGC 4414 is a spiral galaxy, with no bar, and numerous arms. Sc Figure 11.11: NGC 1300 is a spiral galaxy, barred, and with two distinct arms. SBb Figure 11.12: M87 is an elliptical galaxy that is almost entirely spherical. E0. 4. How did Edwin Hubble use Cepheid variables to determine ...
... Figure 11.10: NGC 4414 is a spiral galaxy, with no bar, and numerous arms. Sc Figure 11.11: NGC 1300 is a spiral galaxy, barred, and with two distinct arms. SBb Figure 11.12: M87 is an elliptical galaxy that is almost entirely spherical. E0. 4. How did Edwin Hubble use Cepheid variables to determine ...
Characteristics of Stars
... This is 9.5 trillion km in 1 year Proxima Centauri is 4.2 ly away or 39,900,000,000,000 km or 24.8 trillion miles The circumference of the Earth is ~25,000 miles ...
... This is 9.5 trillion km in 1 year Proxima Centauri is 4.2 ly away or 39,900,000,000,000 km or 24.8 trillion miles The circumference of the Earth is ~25,000 miles ...
Supernovae Oct 19 − Supernova 1987A
... Pre-existing circumstellar ring lit up first by photons from SN, now by blast wave from SN. ...
... Pre-existing circumstellar ring lit up first by photons from SN, now by blast wave from SN. ...
Our Star - the Sun
... Distances to the nearer stars can be determined by parallax, the apparent shift of a star against the background stars observed as the Earth moves along its orbit Parallax measurements made from orbit, above the blurring effects of the atmosphere, are much more accurate than those made with Earth-ba ...
... Distances to the nearer stars can be determined by parallax, the apparent shift of a star against the background stars observed as the Earth moves along its orbit Parallax measurements made from orbit, above the blurring effects of the atmosphere, are much more accurate than those made with Earth-ba ...
LESSON 4, STARS
... red giant, and finally, a white dwarf. A more-massive star: begins as a nebula, becomes a protostar, a main-sequence star, a very massive star, a supergiant, a supernova, and finally, either a neutron star (pulsar) or a black hole. ...
... red giant, and finally, a white dwarf. A more-massive star: begins as a nebula, becomes a protostar, a main-sequence star, a very massive star, a supergiant, a supernova, and finally, either a neutron star (pulsar) or a black hole. ...
Stellar Structure - Astronomy Centre : Research
... • May lose enough mass via winds and superwinds to produce white dwarf and planetary nebula: needs MMS < ~8 M • More massive stars develop core with mass above ...
... • May lose enough mass via winds and superwinds to produce white dwarf and planetary nebula: needs MMS < ~8 M • More massive stars develop core with mass above ...
Supernovae March 23 − Supernova 1987A
... Pre-existing circumstellar ring lit up first by photons from SN, now by blast wave from SN. ...
... Pre-existing circumstellar ring lit up first by photons from SN, now by blast wave from SN. ...
A star is a - Trimble County Schools
... Appear to be tiny specks of white light Most vary in color and are much larger than Earth Motion • Stars move through the night sky towards the west • Stars rotate around the North Star, Polaris – _____________________________ = stars that circle around Polaris • Because of the earth’s rotation, som ...
... Appear to be tiny specks of white light Most vary in color and are much larger than Earth Motion • Stars move through the night sky towards the west • Stars rotate around the North Star, Polaris – _____________________________ = stars that circle around Polaris • Because of the earth’s rotation, som ...
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.