Futuro da Ci^encia no IAG
... observed but should be detected in 2 ways: -High mass stars explode as supernovae and produce a GRBs (z ~ 15 ?) GRB at z~8.2 = pop. III? -First generations of low mass stars should be still evolving, identified by a very low metallicity (or no metals) (z ~ 5 to 15) ...
... observed but should be detected in 2 ways: -High mass stars explode as supernovae and produce a GRBs (z ~ 15 ?) GRB at z~8.2 = pop. III? -First generations of low mass stars should be still evolving, identified by a very low metallicity (or no metals) (z ~ 5 to 15) ...
Document
... If a star’s iron core reaches 1.4 times the mass of the Sun, gravity becomes strong enough to combine electrons and protons into neutrons. During this brief period, heavier elements such as gold and uranium are created, as atomic nuclei are smashed together. The core of the star collapses and ...
... If a star’s iron core reaches 1.4 times the mass of the Sun, gravity becomes strong enough to combine electrons and protons into neutrons. During this brief period, heavier elements such as gold and uranium are created, as atomic nuclei are smashed together. The core of the star collapses and ...
Earths Place in the Universe
... interstellar gas and dust called a nebula Collapses on its self from its own gravity ...
... interstellar gas and dust called a nebula Collapses on its self from its own gravity ...
Activity: Stellar Spectra
... observations table, then click on ‘Give me another star’ and try again. If you got it wrong click on ‘back to the same star’ and try again and then record your results. 7. Repeat for at least 4 different stars. DATA ...
... observations table, then click on ‘Give me another star’ and try again. If you got it wrong click on ‘back to the same star’ and try again and then record your results. 7. Repeat for at least 4 different stars. DATA ...
Stars - HMXEarthScience
... 1. Large clouds of dust and gas are pulled together by gravity (these clouds are called nebulae) 2. Gases in the nebula contract due to gravity, resulting in the formation of a protostar. 3. Pressure and temperature increase until the gases “ignite” and nuclear fusion begins 4. Once the star has ful ...
... 1. Large clouds of dust and gas are pulled together by gravity (these clouds are called nebulae) 2. Gases in the nebula contract due to gravity, resulting in the formation of a protostar. 3. Pressure and temperature increase until the gases “ignite” and nuclear fusion begins 4. Once the star has ful ...
Radio-quiet Isolated Neutron Stars
... Detected in the RASS between 1990/09/14~1990/10/02. Identified with the 1992/10/16 PSPC data. No variability at levels greater than ~1% in 1hr, or <30% on timescale up to 15 years. ...
... Detected in the RASS between 1990/09/14~1990/10/02. Identified with the 1992/10/16 PSPC data. No variability at levels greater than ~1% in 1hr, or <30% on timescale up to 15 years. ...
Announcements - Lick Observatory
... • For stars less than 6Mo these last slides describe the evolution pretty well. There are some differences in the details that depend on the initial main-sequence mass. • For stars that start with > 4Mo, it gets hot enough in the cores to (1) avoid the helium flash and (2) to start carbon fusion. • ...
... • For stars less than 6Mo these last slides describe the evolution pretty well. There are some differences in the details that depend on the initial main-sequence mass. • For stars that start with > 4Mo, it gets hot enough in the cores to (1) avoid the helium flash and (2) to start carbon fusion. • ...
Barium Stars Observed with the Coude Echelle Spectrometer
... The optical counterpart of the pulsating X-ray source H 2252035 appeared to be an interesting object for optical astronomers also. In the X-ray domain it shows the same characterislics as other pulsars. Its X-ray emission is modulated with a period of about 805 s, the pulse amplitude being about 25 ...
... The optical counterpart of the pulsating X-ray source H 2252035 appeared to be an interesting object for optical astronomers also. In the X-ray domain it shows the same characterislics as other pulsars. Its X-ray emission is modulated with a period of about 805 s, the pulse amplitude being about 25 ...
Semester 1 Earth Science Gallery Review
... 4. What color is Deneb? 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 i ...
... 4. What color is Deneb? 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 i ...
Astronomy 120
... a) Calculate the escape velocity from a solar-mass neutron star with a radius of 10 km. b) Do the same thing for a solar-mass, white dwarf star with a radius of 7000 km. 13. Imagine a brown dwarf with a temperature of 1500 K and a radius of 0.1 the sun's radius. If it radiates like a black-body, wha ...
... a) Calculate the escape velocity from a solar-mass neutron star with a radius of 10 km. b) Do the same thing for a solar-mass, white dwarf star with a radius of 7000 km. 13. Imagine a brown dwarf with a temperature of 1500 K and a radius of 0.1 the sun's radius. If it radiates like a black-body, wha ...
Chapter 20
... the subscript, and an atomic mass of 2, which gives the superscript. (Note that 21H is also correct notation.) Deuterium has atomic number equal to 1 and mass number equal to 2. Similarly, 92U238 is an isotope of uranium with 92 protons (atomic number 92) and mass number of 238, which is divided int ...
... the subscript, and an atomic mass of 2, which gives the superscript. (Note that 21H is also correct notation.) Deuterium has atomic number equal to 1 and mass number equal to 2. Similarly, 92U238 is an isotope of uranium with 92 protons (atomic number 92) and mass number of 238, which is divided int ...
Astr604-Ch4
... system must be conserved, any loss in energy when the electron and proton combine to form an atom must come at the expense of a loss in total mass. This is the binding energy of the atom. The estimate of the nuclear timescale for the Sun was based on the assumption that four hydrogen nuclei are conv ...
... system must be conserved, any loss in energy when the electron and proton combine to form an atom must come at the expense of a loss in total mass. This is the binding energy of the atom. The estimate of the nuclear timescale for the Sun was based on the assumption that four hydrogen nuclei are conv ...
Section 4.4: Where did the elements come from?
... Right after the big bang, temperatures were so high that only energy could exist. As the universe expanded, it cooled and protons and neutrons, and electrons condensed out of the energy. Further cooling caused these particles to coalesce into hydrogen and helium atoms. Over time, huge clouds of hydr ...
... Right after the big bang, temperatures were so high that only energy could exist. As the universe expanded, it cooled and protons and neutrons, and electrons condensed out of the energy. Further cooling caused these particles to coalesce into hydrogen and helium atoms. Over time, huge clouds of hydr ...
The structure of the nucleus - Assets
... shelf to the floor: it then has less gravitational potential energy but is in a more stable position. In order to reverse a nuclear reaction we would need to supply energy, just as we would to put the book back on its shelf. Because the energy that is ...
... shelf to the floor: it then has less gravitational potential energy but is in a more stable position. In order to reverse a nuclear reaction we would need to supply energy, just as we would to put the book back on its shelf. Because the energy that is ...
Abstracts 163 MONTE CARL0 SIMULATION OF IN
... Cosmogenic nuclides produced in situ in terrestrial surface samples provide an important tool for dating and determining erosional histories of landforms. Reliable interpretation of the measured nuclide contents requires a good understanding of fundamentals of nuclide production mechanisms. We prese ...
... Cosmogenic nuclides produced in situ in terrestrial surface samples provide an important tool for dating and determining erosional histories of landforms. Reliable interpretation of the measured nuclide contents requires a good understanding of fundamentals of nuclide production mechanisms. We prese ...
File
... White Dwarf-when a star reaches this stage it shines with a white-hot light. Once all the energy is gone, it becomes a Black Dwarf. It will remain without light forever. Supernova –A very large star then explodes, throwing off gas and dust in all directions. 5. After the Supernova stage, the star be ...
... White Dwarf-when a star reaches this stage it shines with a white-hot light. Once all the energy is gone, it becomes a Black Dwarf. It will remain without light forever. Supernova –A very large star then explodes, throwing off gas and dust in all directions. 5. After the Supernova stage, the star be ...
Test 1 - Brock physics
... (c) remains constant as time passes. (d) [Pulsars do not spin.] 34. The Schwarzschild radius is (a) the smallest possible radius of a white dwarf. (b) the smallest possible radius of a neutron star. (c) the radius of the region around a neutron star within which X-ray bursts occur. (d) the radius of ...
... (c) remains constant as time passes. (d) [Pulsars do not spin.] 34. The Schwarzschild radius is (a) the smallest possible radius of a white dwarf. (b) the smallest possible radius of a neutron star. (c) the radius of the region around a neutron star within which X-ray bursts occur. (d) the radius of ...
Nucleosynthesis, the r-Process, Abundances and Jim Truran
... Cameron & Truran (1977) The Supernova Trigger for the Formation of the Solar System Truran, Cowan & Cameron (1978) The Helium Driven rProcess in Supernovae Truran (1981) A New Interpretation of the Heavy Element Abundances in Metal-deficient Stars Cowan, Thielemann & Truran (1991) The r-Process and ...
... Cameron & Truran (1977) The Supernova Trigger for the Formation of the Solar System Truran, Cowan & Cameron (1978) The Helium Driven rProcess in Supernovae Truran (1981) A New Interpretation of the Heavy Element Abundances in Metal-deficient Stars Cowan, Thielemann & Truran (1991) The r-Process and ...
RED GIANTS
... Missing the Main Sequence • If the protostar has a mass < 0.08 M: – It does not contain enough gravitational energy to reach a core temperature of 107 K – No fusion reactions occur – The star is stillborn! ...
... Missing the Main Sequence • If the protostar has a mass < 0.08 M: – It does not contain enough gravitational energy to reach a core temperature of 107 K – No fusion reactions occur – The star is stillborn! ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.