ppt - Astronomy & Physics
... So net result is conversion of 4 protons into Helium nucleus. The mass of the Helium nucleus is less than the mass of the 4 protons, and this mass is converted into energy, which powers the Sun (and other stars) ...
... So net result is conversion of 4 protons into Helium nucleus. The mass of the Helium nucleus is less than the mass of the 4 protons, and this mass is converted into energy, which powers the Sun (and other stars) ...
Take time to understand it now
... • Come to a consensus answer you both agree on. • If you get stuck or are not sure of your answer, ask ...
... • Come to a consensus answer you both agree on. • If you get stuck or are not sure of your answer, ask ...
1 Ay 124 Winter 2016 – HOMEWORK #3
... Due Friday, Feb 5, 2016 by 5pm, in Denise’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about t ...
... Due Friday, Feb 5, 2016 by 5pm, in Denise’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about t ...
star-formation rate
... Galaxies do not become very red if τ is large because their star formation rate, and thus the fraction of massive blue stars, does not decrease sufficiently. ...
... Galaxies do not become very red if τ is large because their star formation rate, and thus the fraction of massive blue stars, does not decrease sufficiently. ...
Other Galaxies, their Distances, and the Expansion of the Universe
... Some galaxies even show evidence for very violent ejection of material into the intergalactic space ...
... Some galaxies even show evidence for very violent ejection of material into the intergalactic space ...
What`s Up - April 2016
... brighter one is about half again as bright as our sun, the fainter about half as bright as the sun. Separated by about 23 times the distance from the Earth to the sun, they take 80 years to orbit each other. For many years it was believed that these were the two nearest stars to our own sun. But a t ...
... brighter one is about half again as bright as our sun, the fainter about half as bright as the sun. Separated by about 23 times the distance from the Earth to the sun, they take 80 years to orbit each other. For many years it was believed that these were the two nearest stars to our own sun. But a t ...
Astronomy Library wk 6.cwk (WP)
... As a body is heated, the peak intensity occurs at shorter (more energetic) wavelengths. ...
... As a body is heated, the peak intensity occurs at shorter (more energetic) wavelengths. ...
Jeopardy - University of Nebraska–Lincoln
... become after blowing off their outer layers in a planetary nebula. ...
... become after blowing off their outer layers in a planetary nebula. ...
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... • The brightest and bluest, OB stars explode within a few million years, and thus don’t go far from the spiral arm where they were born ...
... • The brightest and bluest, OB stars explode within a few million years, and thus don’t go far from the spiral arm where they were born ...
File
... center becomes hot enough to begin the fusion of hydrogen into helium. A main sequence star has now been born, and will spend the next 90% of its life in this stage. When all of the hydrogen has been fused, the star initially collapses, but then gets hot enough in its core to fuse helium into carbon ...
... center becomes hot enough to begin the fusion of hydrogen into helium. A main sequence star has now been born, and will spend the next 90% of its life in this stage. When all of the hydrogen has been fused, the star initially collapses, but then gets hot enough in its core to fuse helium into carbon ...
Name _________ Date _____________ Period ______ Skills
... d. their size. _____ 18. Stars are now classified by a. their elements. b. their temperature. c. their age. d. their size. _____ 19. Class O stars, the hottest stars, are a. yellow. b. orange. c. red. d. blue. 20. Early astronomers called the brightest stars in the sky ______________________ stars. ...
... d. their size. _____ 18. Stars are now classified by a. their elements. b. their temperature. c. their age. d. their size. _____ 19. Class O stars, the hottest stars, are a. yellow. b. orange. c. red. d. blue. 20. Early astronomers called the brightest stars in the sky ______________________ stars. ...
Semester 1 Earth Science Gallery Review
... 5. What temperature is Sirius B? 6. This star is a red Giant. 7. What temperature is Bernard’s Star? 8. Which star is the dimmest (least bright) on the chart? 9. What category is the hottest star on the chart? 10. What color are the coolest stars? 11. What category of stars is hot but not very lumin ...
... 5. What temperature is Sirius B? 6. This star is a red Giant. 7. What temperature is Bernard’s Star? 8. Which star is the dimmest (least bright) on the chart? 9. What category is the hottest star on the chart? 10. What color are the coolest stars? 11. What category of stars is hot but not very lumin ...
1 Ay 124 Winter 2014 – HOMEWORK #3
... Due Friday, Feb 14, 2014 by 5pm, in Steidel’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about ...
... Due Friday, Feb 14, 2014 by 5pm, in Steidel’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about ...
1_Introduction
... Universe was denser in the past; if we daringly extrapolate backward to infinite density, that was a finite time ago. ...
... Universe was denser in the past; if we daringly extrapolate backward to infinite density, that was a finite time ago. ...
Elemental Abundances
... Iron Group • Fe-group elements represent approximate nuclear statistical equilibrium at T ≈109 K • Result of shock that emerges from the core of a massive star that has collapsed into a neutron star (SN II) OR sudden ignition of C in a white dwarf that has accreted enough material from a companion ...
... Iron Group • Fe-group elements represent approximate nuclear statistical equilibrium at T ≈109 K • Result of shock that emerges from the core of a massive star that has collapsed into a neutron star (SN II) OR sudden ignition of C in a white dwarf that has accreted enough material from a companion ...
Stages 12 to 14
... The carbon rich core continues to contract and heat up. Carbon fusion requires a temperature of 500 to 600 million K. The core will contract until electron degeneracy pressure once again takes over, and contraction ends If the star is similar to the sun, the mass is too small, the ignition temperatu ...
... The carbon rich core continues to contract and heat up. Carbon fusion requires a temperature of 500 to 600 million K. The core will contract until electron degeneracy pressure once again takes over, and contraction ends If the star is similar to the sun, the mass is too small, the ignition temperatu ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.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.