Fundamentals of Atmospheric Chemistry and Astrochemistry
... existed in nature in the instant after the big bang. However, it appears that it can be recreated in high energy collision experiments such as those being carried out at the Large Hadron Collider at CERN. ...
... existed in nature in the instant after the big bang. However, it appears that it can be recreated in high energy collision experiments such as those being carried out at the Large Hadron Collider at CERN. ...
WG4: Nuclear Astrophysics
... The Life Cycle of Matter Cosmic gas is collected by gravitational attraction into higher density regions, to eventually form stars of different masses. These stars are stabilised against further gravitational concentration by the release of nuclear binding energy in their interiors. Depending on the ...
... The Life Cycle of Matter Cosmic gas is collected by gravitational attraction into higher density regions, to eventually form stars of different masses. These stars are stabilised against further gravitational concentration by the release of nuclear binding energy in their interiors. Depending on the ...
Life Stages of High
... carbon in a shell around the carbon core, and H fuses to He in a shell around the helium layer • This double-shell burning stage never reaches equilibrium—fusion rate periodically spikes upward in a series of thermal pulses • With each spike, convection dredges carbon up from core and transports it ...
... carbon in a shell around the carbon core, and H fuses to He in a shell around the helium layer • This double-shell burning stage never reaches equilibrium—fusion rate periodically spikes upward in a series of thermal pulses • With each spike, convection dredges carbon up from core and transports it ...
How Did We Wind Up in Such an Unlikely Universe?
... than elsewhere and pull surrounding gas into a collapsing ball. As it collapsed it got hot enough so that nuclear fusion started. The first stars were born. When the first stars died they seeded the galaxies in which they existed with lots of higher atomic number atoms that had been cooked up throug ...
... than elsewhere and pull surrounding gas into a collapsing ball. As it collapsed it got hot enough so that nuclear fusion started. The first stars were born. When the first stars died they seeded the galaxies in which they existed with lots of higher atomic number atoms that had been cooked up throug ...
Stars, Galaxies, and the Universe
... Telescopes: Collect and focus different types of electromagnetic radiation including visible light. Convex lens: A piece of transparent glass, curved so that the middle is thicker than the edges. Refracting telescopes: use convex lens to gather a large amount of light and focus it into a small area. ...
... Telescopes: Collect and focus different types of electromagnetic radiation including visible light. Convex lens: A piece of transparent glass, curved so that the middle is thicker than the edges. Refracting telescopes: use convex lens to gather a large amount of light and focus it into a small area. ...
Beyond the iron group: heavy metals in hot subdwarfs
... three resonance lines of Zr iv, as well as Zn iv and possibly Cd iv are present in at least Feige 66, however no oscillator strengths for these lines could be found in the literature. We note that the only other report of these resonance lines in UV spectra was by Proffitt et al. (2001), who discuss ...
... three resonance lines of Zr iv, as well as Zn iv and possibly Cd iv are present in at least Feige 66, however no oscillator strengths for these lines could be found in the literature. We note that the only other report of these resonance lines in UV spectra was by Proffitt et al. (2001), who discuss ...
Chapter 2
... • Energy from Big Bang transformed into matter (more details of this matter/energy relationship in Chapter 21). • Fusing of fundamental/subatomic particles (protons/neutrons) created atomic nuclei. ...
... • Energy from Big Bang transformed into matter (more details of this matter/energy relationship in Chapter 21). • Fusing of fundamental/subatomic particles (protons/neutrons) created atomic nuclei. ...
Balloon Model of the Life Cycle of Stars
... the very large blue and red balloons as large as possible without popping them. ...
... the very large blue and red balloons as large as possible without popping them. ...
100 Greatest Discoveries - Mr-Hubeny
... The “extra” 3-4 degrees measured by Wilson and Penzias showed energy that was left over from the Big Bang theory. 11. Gamma-Ray Bursts (1969 – 1997) The two-decade-long mystery of gamma-ray bursts is solved by a host of sophisticated ground-based and orbiting telescopes. Gamma-ray bursts are short-l ...
... The “extra” 3-4 degrees measured by Wilson and Penzias showed energy that was left over from the Big Bang theory. 11. Gamma-Ray Bursts (1969 – 1997) The two-decade-long mystery of gamma-ray bursts is solved by a host of sophisticated ground-based and orbiting telescopes. Gamma-ray bursts are short-l ...
High School Conceptual Progressions Model Course II – Bundle 1
... HS-ESS1-3). An example is the star called the sun, which is changing and will burn out over a lifespan of approximately 10 billion years (ESS1.A as in HSESS1-1). Other than the hydrogen and helium formed at the time of the Big Bang, nuclear fusion within stars produces all atomic nuclei lighter than ...
... HS-ESS1-3). An example is the star called the sun, which is changing and will burn out over a lifespan of approximately 10 billion years (ESS1.A as in HSESS1-1). Other than the hydrogen and helium formed at the time of the Big Bang, nuclear fusion within stars produces all atomic nuclei lighter than ...
Beyond the iron group: Heavy metals in hot subdwarfs
... appear to be unidentified. While analysing our HST/STIS spectra we noticed that the wavelengths of two very strong unmatched lines corresponded very well with the resonance doublet of Ge . The region around the line at 1189.028 Å is shown in Fig. 2 (the other line is at 1229.840 Å). There are no s ...
... appear to be unidentified. While analysing our HST/STIS spectra we noticed that the wavelengths of two very strong unmatched lines corresponded very well with the resonance doublet of Ge . The region around the line at 1189.028 Å is shown in Fig. 2 (the other line is at 1229.840 Å). There are no s ...
Where Stars Are Born
... 6. No emission nebula would be found around the Sun (which is in fact surrounded by gas) because the Sun is too cool to produce the large numbers of UV photons required to energize the gas of an emission nebula. 7. i) Collision between clouds. ii) Compression of a cloud by a nearby emission nebula ...
... 6. No emission nebula would be found around the Sun (which is in fact surrounded by gas) because the Sun is too cool to produce the large numbers of UV photons required to energize the gas of an emission nebula. 7. i) Collision between clouds. ii) Compression of a cloud by a nearby emission nebula ...
Stars - Barrington 220
... The stars have been explored a lot, but there is still so much more that we can do with the exploration of stars that we know is possible, but some things we can not achieve with the technology we have today, but in the future who knows what we can do with exploring the stars! And I hope that the li ...
... The stars have been explored a lot, but there is still so much more that we can do with the exploration of stars that we know is possible, but some things we can not achieve with the technology we have today, but in the future who knows what we can do with exploring the stars! And I hope that the li ...
NEUTRON STARS AND PULSARS Discovery Were it not for
... place involving the production of ever heavier nuclei until iron and nickel are made. The process ends here because the fusion of heavier nuclei does not put out energy; it requires an input of energy. In low mass stars, because gravity is weak, these processes proceed very slowly. Our sun will live ...
... place involving the production of ever heavier nuclei until iron and nickel are made. The process ends here because the fusion of heavier nuclei does not put out energy; it requires an input of energy. In low mass stars, because gravity is weak, these processes proceed very slowly. Our sun will live ...
Wind Opacity Issues
... crude. And it makes me wonder what elements are included in the calculation of the overall opacity and how reliable the smooth portions of the curves are. As you look at the figures in this document, keep in mind that some plot cross section and some plot the radius of optical depth unity, R1. R1 is ...
... crude. And it makes me wonder what elements are included in the calculation of the overall opacity and how reliable the smooth portions of the curves are. As you look at the figures in this document, keep in mind that some plot cross section and some plot the radius of optical depth unity, R1. R1 is ...
(1) and
... (1) To specialist (astronomer) = OK What are Chandrasekhar mass, Hubble constant, Stellar structure, SN and SNR. (2) To general public (citizen) = OK Big bang, Black hole Between (1) and (2) is very difficult. My talk is limited area of Astronomy : Hot plasma and Nucleosynthesis in SNRs ...
... (1) To specialist (astronomer) = OK What are Chandrasekhar mass, Hubble constant, Stellar structure, SN and SNR. (2) To general public (citizen) = OK Big bang, Black hole Between (1) and (2) is very difficult. My talk is limited area of Astronomy : Hot plasma and Nucleosynthesis in SNRs ...
Testing - Elon University
... A. They’re stuck to interstellar medium B. Gravity of disk stars pulls toward disk C. Halo stars knock them back into disk ...
... A. They’re stuck to interstellar medium B. Gravity of disk stars pulls toward disk C. Halo stars knock them back into disk ...
AY2 - Overview of the Universe
... A) Without more information, it is impossible to know how fast you would see a light beam from Earth coming toward you. If it happens that you are going fast enough so that the light can't catch you, then people on Earth would find you to be going faster than light. B) An imaginary spaceship can go ...
... A) Without more information, it is impossible to know how fast you would see a light beam from Earth coming toward you. If it happens that you are going fast enough so that the light can't catch you, then people on Earth would find you to be going faster than light. B) An imaginary spaceship can go ...
Characteristics of Stars
... imagined that groups of stars formed pictures of people or animals. Today, we call these imaginary patterns of stars constellations. Astronomers classify stars according to their physical characteristics. Characteristics used to classify stars include color, temperature, size, composition, and brigh ...
... imagined that groups of stars formed pictures of people or animals. Today, we call these imaginary patterns of stars constellations. Astronomers classify stars according to their physical characteristics. Characteristics used to classify stars include color, temperature, size, composition, and brigh ...
THE PRIMORDIAL HELIUM ABUNDANCE Manuel Peimbert
... The homogeneous model of the expansion of the universe based on the general theory of relativity, now known as the Big Bang Theory (BBT), predicts that during the first four minutes, counted from the beginning of the expansion of the universe, there were nuclear reactions based on hydrogen that prod ...
... The homogeneous model of the expansion of the universe based on the general theory of relativity, now known as the Big Bang Theory (BBT), predicts that during the first four minutes, counted from the beginning of the expansion of the universe, there were nuclear reactions based on hydrogen that prod ...
Neutron Star Formation
... PdV work: The initial ejecta decelerates as it drives an explosion through the star. If the velocity decelerates below the escape velocity, it falls back (Fryer 1999): Accretion happens quickly (first 100s) Reverse shock: The shock decelerates in the flat density gradient of the envelope, drivin ...
... PdV work: The initial ejecta decelerates as it drives an explosion through the star. If the velocity decelerates below the escape velocity, it falls back (Fryer 1999): Accretion happens quickly (first 100s) Reverse shock: The shock decelerates in the flat density gradient of the envelope, drivin ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... The evolution of massive stars have the following general characteristics and differences to lower mass evolution 1. The electrons in their cores do not become degenerate until the final burning stages, when iron core is reached 2. Mass-loss plays an important role in the entire evolution (we will c ...
... The evolution of massive stars have the following general characteristics and differences to lower mass evolution 1. The electrons in their cores do not become degenerate until the final burning stages, when iron core is reached 2. Mass-loss plays an important role in the entire evolution (we will c ...
Powerpoint
... For helium burning, there is no effect around 10 solar mases, but the higher masses have a longer lifetime with higher metallicity because mass loss decreases the mass. For lower masses, there is a significant metallicity dependence for the helium burning lifetime. The reason is not clear. Perhaps ...
... For helium burning, there is no effect around 10 solar mases, but the higher masses have a longer lifetime with higher metallicity because mass loss decreases the mass. For lower masses, there is a significant metallicity dependence for the helium burning lifetime. The reason is not clear. Perhaps ...
ASTRONOMY 0089: EXAM 2 Class Meets M,W,F, 1:00 PM Mar 22
... a. are evolved low-mass stars burning He in their core. b. are stars of extremely low mass whose central temperature never gets high enough to initiate the fusion of H into He. c. are extremely young objects approaching the Main Sequence. d. are a form of pulsating star useful for determining stella ...
... a. are evolved low-mass stars burning He in their core. b. are stars of extremely low mass whose central temperature never gets high enough to initiate the fusion of H into He. c. are extremely young objects approaching the Main Sequence. d. are a form of pulsating star useful for determining stella ...
Nucleosynthesis
Nucleosynthesis is the process that creates new atomic nuclei from pre-existing nucleons, primarily protons and neutrons. The first nuclei were formed about three minutes after the Big Bang, through the process called Big Bang nucleosynthesis. It was then that hydrogen and helium formed to become the content of the first stars, and this primeval process is responsible for the present hydrogen/helium ratio of the cosmos.With the formation of stars, heavier nuclei were created from hydrogen and helium by stellar nucleosynthesis, a process that continues today. Some of these elements, particularly those lighter than iron, continue to be delivered to the interstellar medium when low mass stars eject their outer envelope before they collapse to form white dwarfs. The remains of their ejected mass form the planetary nebulae observable throughout our galaxy.Supernova nucleosynthesis within exploding stars by fusing carbon and oxygen is responsible for the abundances of elements between magnesium (atomic number 12) and nickel (atomic number 28). Supernova nucleosynthesis is also thought to be responsible for the creation of rarer elements heavier than iron and nickel, in the last few seconds of a type II supernova event. The synthesis of these heavier elements absorbs energy (endothermic) as they are created, from the energy produced during the supernova explosion. Some of those elements are created from the absorption of multiple neutrons (the R process) in the period of a few seconds during the explosion. The elements formed in supernovas include the heaviest elements known, such as the long-lived elements uranium and thorium.Cosmic ray spallation, caused when cosmic rays impact the interstellar medium and fragment larger atomic species, is a significant source of the lighter nuclei, particularly 3He, 9Be and 10,11B, that are not created by stellar nucleosynthesis.In addition to the fusion processes responsible for the growing abundances of elements in the universe, a few minor natural processes continue to produce very small numbers of new nuclides on Earth. These nuclides contribute little to their abundances, but may account for the presence of specific new nuclei. These nuclides are produced via radiogenesis (decay) of long-lived, heavy, primordial radionuclides such as uranium and thorium. Cosmic ray bombardment of elements on Earth also contribute to the presence of rare, short-lived atomic species called cosmogenic nuclides.