DoAr21_AAS2005 - Astronomy at Swarthmore College
... high densities (~ 1013 cm-3). The naked T Tauri star HD 98800 shows large f/i ratios, indicating low densities. Our Chandra observations of DoAr 21 show intermediate f/i ratios for Si (right) and S. The implied densities are more in-line with the high values seen in TW Hya, but our results have larg ...
... high densities (~ 1013 cm-3). The naked T Tauri star HD 98800 shows large f/i ratios, indicating low densities. Our Chandra observations of DoAr 21 show intermediate f/i ratios for Si (right) and S. The implied densities are more in-line with the high values seen in TW Hya, but our results have larg ...
Lives of stars HR
... produce internal pressure with fusion reactions; the Sun runs out of energy. The envelope is ejected, and the core of the Sun forms a very dense, solid white dwarf star. A famous planetary nebula with a white dwarf in the center is M57 ...
... produce internal pressure with fusion reactions; the Sun runs out of energy. The envelope is ejected, and the core of the Sun forms a very dense, solid white dwarf star. A famous planetary nebula with a white dwarf in the center is M57 ...
Part 1
... Below are two star photos taken six months apart and laid atop one another so the background stars (circles) line up. There are two nearby stars also shown. Which of these nearby stars is closer? ...
... Below are two star photos taken six months apart and laid atop one another so the background stars (circles) line up. There are two nearby stars also shown. Which of these nearby stars is closer? ...
How Close is our Nearest Neighbor
... When Shapley did his experiment, he had to measure the distances to globular clusters. To do this, he used Henrietta Leavitt’s discovery that certain variable stars obeyed a period-luminosity law so that their luminosities could be determined by measuring their periods of variation. These variable s ...
... When Shapley did his experiment, he had to measure the distances to globular clusters. To do this, he used Henrietta Leavitt’s discovery that certain variable stars obeyed a period-luminosity law so that their luminosities could be determined by measuring their periods of variation. These variable s ...
Stars are made of very hot gas. This gas is mostly hydrogen and
... to live a very long time. Some red dwarf stars will live trillions of years before they run out of fuel Why are red dwarf stars red? Because red dwarf stars only burn a little bit of fuel at a time, they are not very hot compared to other stars. Think of a fire. The coolest part of the fire at the t ...
... to live a very long time. Some red dwarf stars will live trillions of years before they run out of fuel Why are red dwarf stars red? Because red dwarf stars only burn a little bit of fuel at a time, they are not very hot compared to other stars. Think of a fire. The coolest part of the fire at the t ...
star-formation rate
... about 4000 Å which becomes visible in the spectrum after a few 107 years. This break is caused by a strongly changing opacity of stellar atmospheres at this wavelength, mainly due to strong transitions of singly ionized calcium and the Balmer lines of hydrogen. ...
... about 4000 Å which becomes visible in the spectrum after a few 107 years. This break is caused by a strongly changing opacity of stellar atmospheres at this wavelength, mainly due to strong transitions of singly ionized calcium and the Balmer lines of hydrogen. ...
Lives of Stars - Amazon Web Services
... Neutron Stars After a supergiant explodes, some of the material from the star is left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. They are even smaller and denser than white dwarfs. A neutron star may contain as much as three times the mass of the ...
... Neutron Stars After a supergiant explodes, some of the material from the star is left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. They are even smaller and denser than white dwarfs. A neutron star may contain as much as three times the mass of the ...
Chapter 12: Measuring the Properties of Stars
... 1. More than half of what appear as single stars are, in fact, multiple star systems. 2. Optical doubles are two stars that have small angular separation as seen from Earth but are not gravitationally linked. 3. A binary star system is a system of two stars that are gravitationally linked so that th ...
... 1. More than half of what appear as single stars are, in fact, multiple star systems. 2. Optical doubles are two stars that have small angular separation as seen from Earth but are not gravitationally linked. 3. A binary star system is a system of two stars that are gravitationally linked so that th ...
(Mike Riddle CTI)-84_eng_cr_v4.0
... accepted’ theory of stellar formation may be one of a hundred unsupported dogmas which constitute a large part of present-day ...
... accepted’ theory of stellar formation may be one of a hundred unsupported dogmas which constitute a large part of present-day ...
Long Ago and Far Away
... infrared telescope in astronomy. Figure 2 shows distant galaxies as seen by Spitzer in infrared light and by the Hubble Space Telescope (HST) in visible light. HST makes distant galaxies look almost nearby! But some infrared-bright galaxies are hard to see in the HST image, because dust obscures vis ...
... infrared telescope in astronomy. Figure 2 shows distant galaxies as seen by Spitzer in infrared light and by the Hubble Space Telescope (HST) in visible light. HST makes distant galaxies look almost nearby! But some infrared-bright galaxies are hard to see in the HST image, because dust obscures vis ...
HR Diagram, Star Clusters, and Stellar Evolution
... • A RG brightens by a factor of between 1,000 and 10,000. The outer, hydrogen-rich envelope swells up to a few au radius, with T ~ 2,000 - 3,000 K • A strong stellar wind begins to blow from the star's surface (akin to the Sun's solar wind, but much stronger), and, in the course of the star's RG l ...
... • A RG brightens by a factor of between 1,000 and 10,000. The outer, hydrogen-rich envelope swells up to a few au radius, with T ~ 2,000 - 3,000 K • A strong stellar wind begins to blow from the star's surface (akin to the Sun's solar wind, but much stronger), and, in the course of the star's RG l ...
key - Scioly.org
... 34) SS Cygni (8 points) a) 372 light years b) 520 light years; the period of the star’s fluctuations did not match with the predicted distance (2 points) c) Cataclysmic d) Cataclysmic variable stars are binary systems in which one white dwarf accretes mass from another star. (1 point). When the accr ...
... 34) SS Cygni (8 points) a) 372 light years b) 520 light years; the period of the star’s fluctuations did not match with the predicted distance (2 points) c) Cataclysmic d) Cataclysmic variable stars are binary systems in which one white dwarf accretes mass from another star. (1 point). When the accr ...
Test 1, Feb. 2, 2016 - Brock physics
... 29. The maximum mass that a white dwarf can have is (a) 0.14 solar masses. (b) 1.4 solar masses. (c) 14 solar masses. (d) [The statement is wrong. A white dwarf can have any mass.] 30. Which of the following nuclei has the lowest binding energy per nucleon? (a) The nucleus of helium. (b) The nucleus ...
... 29. The maximum mass that a white dwarf can have is (a) 0.14 solar masses. (b) 1.4 solar masses. (c) 14 solar masses. (d) [The statement is wrong. A white dwarf can have any mass.] 30. Which of the following nuclei has the lowest binding energy per nucleon? (a) The nucleus of helium. (b) The nucleus ...
Active Galactic Nuclei: are they important?
... surrounded by plentiful material flowing in and out •This material emits radiation so we can trace what is happening close to a black hole ...
... surrounded by plentiful material flowing in and out •This material emits radiation so we can trace what is happening close to a black hole ...
DSLR photometry - British Astronomical Association
... to measure multiple stars in the field of view By using a normal camera lens or small telephoto lenses (50mm-300mm), bright stars can be measured that are too bright for a CCD camera with a telescope. The scatter from visual observers is usually about 0.2-0.5 mag, but in DSLR measurements the scatte ...
... to measure multiple stars in the field of view By using a normal camera lens or small telephoto lenses (50mm-300mm), bright stars can be measured that are too bright for a CCD camera with a telescope. The scatter from visual observers is usually about 0.2-0.5 mag, but in DSLR measurements the scatte ...
ASTR 1120-001 Final Examination Phil Armitage, Bruce Ferguson
... (a) Galaxies (except very nearby ones) were moving away from you, with the most distant ones moving away the slowest (b) Galaxies are moving toward you, with the most distant ones approaching the most rapidly (c) Galaxies are moving toward you, with the most distant ones approaching the slowest 68. ...
... (a) Galaxies (except very nearby ones) were moving away from you, with the most distant ones moving away the slowest (b) Galaxies are moving toward you, with the most distant ones approaching the most rapidly (c) Galaxies are moving toward you, with the most distant ones approaching the slowest 68. ...
File
... such high temperatures that nuclear fusion begins again. This time, carbon atoms in the core fuse into heavier elements until the core is almost entirely made of iron. • When nuclear fusion stops, the star’s core begins to collapse under its own gravity. This causes the outer layers to explode outwa ...
... such high temperatures that nuclear fusion begins again. This time, carbon atoms in the core fuse into heavier elements until the core is almost entirely made of iron. • When nuclear fusion stops, the star’s core begins to collapse under its own gravity. This causes the outer layers to explode outwa ...
Multiple Choice, continued
... such high temperatures that nuclear fusion begins again. This time, carbon atoms in the core fuse into heavier elements until the core is almost entirely made of iron. • When nuclear fusion stops, the star’s core begins to collapse under its own gravity. This causes the outer layers to explode outwa ...
... such high temperatures that nuclear fusion begins again. This time, carbon atoms in the core fuse into heavier elements until the core is almost entirely made of iron. • When nuclear fusion stops, the star’s core begins to collapse under its own gravity. This causes the outer layers to explode outwa ...
PHYSICS 1500 - ASTRONOMY TOTAL: 100 marks Section A Please
... (a) These are clearly the most common type of planet. (b) Smaller, rocky planets always lie closer to the star but are undetectable. (c) Few planetary systems have giant planets more than 1 AU from the star. (d) Detection of less massive planets is currently very difficult. (e) Detection of planets ...
... (a) These are clearly the most common type of planet. (b) Smaller, rocky planets always lie closer to the star but are undetectable. (c) Few planetary systems have giant planets more than 1 AU from the star. (d) Detection of less massive planets is currently very difficult. (e) Detection of planets ...
Chapter 30 Notes
... Supergiants- Stars more massive (not bigger, but have more mass) than our sun, will become larger giants in their third stage. These highly luminous stars are called supergiants. These stars appear along the top of the H-R diagram above. Planetary Nebulas As the star’s outer gases drift away; the re ...
... Supergiants- Stars more massive (not bigger, but have more mass) than our sun, will become larger giants in their third stage. These highly luminous stars are called supergiants. These stars appear along the top of the H-R diagram above. Planetary Nebulas As the star’s outer gases drift away; the re ...
Stars
... stays at this level for weeks as ionized atoms recombine with electrons. After recombination, the gas is not hot enough to be luminous on its own. Now radioactive decay provides a heat source. Both Type I and Type II supernovae produce large amounts of radioactive 56Co (cobalt), which decays to iron ...
... stays at this level for weeks as ionized atoms recombine with electrons. After recombination, the gas is not hot enough to be luminous on its own. Now radioactive decay provides a heat source. Both Type I and Type II supernovae produce large amounts of radioactive 56Co (cobalt), which decays to iron ...
Neutron Stars
... • Our atoms were once parts of stars that died more than 4.6 billion years ago, whose remains were swept up into the solar system when the Sun formed ...
... • Our atoms were once parts of stars that died more than 4.6 billion years ago, whose remains were swept up into the solar system when the Sun formed ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.