Star Light, Star Bright
... How many stars can you see on a clear night? About 5,000 stars are visible from Earth without the use of a telescope, but you can only see a fraction of them from any particular viewing point at any particular time. With the help of a powerful telescope, it's possible to see more than 3 billion of t ...
... How many stars can you see on a clear night? About 5,000 stars are visible from Earth without the use of a telescope, but you can only see a fraction of them from any particular viewing point at any particular time. With the help of a powerful telescope, it's possible to see more than 3 billion of t ...
Ecosystems, from life, to the Earth, to the Galaxy
... independently of another. For instance, even geological processes are influenced by carbon deposition in limestone, built-up ultimately from that provided by the biota, as part of the endogenic cycle. The Gaia hypothesis (Lovelock 1995) has often been misinterpreted as implying that the Earth is ali ...
... independently of another. For instance, even geological processes are influenced by carbon deposition in limestone, built-up ultimately from that provided by the biota, as part of the endogenic cycle. The Gaia hypothesis (Lovelock 1995) has often been misinterpreted as implying that the Earth is ali ...
Stars Part Two
... How do we know all this? By observing Globular clusters… 1. Globular clusters are thousands of stars that all formed at more or less the same time. 2. Globular clusters are much smaller than galaxies. 3. Galaxies create stars in an on-going process. 4. The stars in a globular cluster accrete sudde ...
... How do we know all this? By observing Globular clusters… 1. Globular clusters are thousands of stars that all formed at more or less the same time. 2. Globular clusters are much smaller than galaxies. 3. Galaxies create stars in an on-going process. 4. The stars in a globular cluster accrete sudde ...
9 - WordPress.com
... principles of physics. Our understanding of the cosmos draws upon models, theories and laws in our endeavour to seek explanations for the myriad of observations made by various instruments at many different wavelengths. Techniques, such as imaging, photometry, astrometry and spectroscopy, allow us t ...
... principles of physics. Our understanding of the cosmos draws upon models, theories and laws in our endeavour to seek explanations for the myriad of observations made by various instruments at many different wavelengths. Techniques, such as imaging, photometry, astrometry and spectroscopy, allow us t ...
Nuclear reactions and stellar processes
... nuclei are eventually transported by sequences of convective dredge-up processes from the burning zones to the stellar atmosphere followed by mass loss due to radiation-pressure-driven winds. This scenario often forms planetary nebulae, observed as vast gas clouds surrounding a centre star. Alternat ...
... nuclei are eventually transported by sequences of convective dredge-up processes from the burning zones to the stellar atmosphere followed by mass loss due to radiation-pressure-driven winds. This scenario often forms planetary nebulae, observed as vast gas clouds surrounding a centre star. Alternat ...
Name: Period: _____ Date: 8th Grade Fall Semester Exam Review
... Name: _______________________________________________ Period: _____ Date: ________________ C. near the top, right of the table D. in group 18, the noble gases 24. The elements that are located along the stair-step line of the periodic table are A. metals. B. metalloids. C. nonmetals. D. noble gases ...
... Name: _______________________________________________ Period: _____ Date: ________________ C. near the top, right of the table D. in group 18, the noble gases 24. The elements that are located along the stair-step line of the periodic table are A. metals. B. metalloids. C. nonmetals. D. noble gases ...
Nucleosynthesis of heavy elements in gamma ray bursts
... explosion. Because the non-radioactive material only lights up after the explosion, it does not offer a direct look at the blast itself. ...
... explosion. Because the non-radioactive material only lights up after the explosion, it does not offer a direct look at the blast itself. ...
5.2.1 Doppler Hubble Toil and Trouble
... to production of protons and antiprotons, and electrons and positrons. Somehow (and this is one of the biggest questions in physics today), we ended up in a universe with only matter. We think that there was a tiny asymmetry in the matter-antimatter production. (If there hadn’t been, we couldn’t ...
... to production of protons and antiprotons, and electrons and positrons. Somehow (and this is one of the biggest questions in physics today), we ended up in a universe with only matter. We think that there was a tiny asymmetry in the matter-antimatter production. (If there hadn’t been, we couldn’t ...
Virtual practice and Spectroscopy lab 3/7/10
... In the flame test you saw a single color as the excited atoms released the energy they gained. But there are billions of excited atoms releasing energy. The excited atoms do not all emit the same energy light because the amount of energy that excited them may differ. The kinds of light energy that c ...
... In the flame test you saw a single color as the excited atoms released the energy they gained. But there are billions of excited atoms releasing energy. The excited atoms do not all emit the same energy light because the amount of energy that excited them may differ. The kinds of light energy that c ...
origins powerpoint
... about 10-35 second after the big bang when it became so cool that the forces of nature caused the universe to inflate tremendously. • The initial expansion was faster than the speed of light. • The universe is still expanding today. ...
... about 10-35 second after the big bang when it became so cool that the forces of nature caused the universe to inflate tremendously. • The initial expansion was faster than the speed of light. • The universe is still expanding today. ...
Effects of triple-α and C(α, γ )16 O reaction rates on the supernova
... the production of 12 C and 16 O proceeds appreciably and these elements should become the main products after core He-burning in all massive stars. From core C-burning to the end of core oxygen burning, carbon continues to decrease little by little due to shell burnings. This fact is almost universa ...
... the production of 12 C and 16 O proceeds appreciably and these elements should become the main products after core He-burning in all massive stars. From core C-burning to the end of core oxygen burning, carbon continues to decrease little by little due to shell burnings. This fact is almost universa ...
Chemical Evolution of the Galaxy and its satellites
... • The SFR is the star formation rate (how many solar masses go into stars per unit time) • The IMF is the initial stellar mass function describing the distribution of stars as a function of stellar mass ...
... • The SFR is the star formation rate (how many solar masses go into stars per unit time) • The IMF is the initial stellar mass function describing the distribution of stars as a function of stellar mass ...
Chapter 15. The Chandrasekhar Limit, Iron-56 and Core
... speed of light. The light from the supernova, although a mere 1% or so of its total energy, nonetheless may be enough to outshine its entire galaxy for a period of days or weeks. This is a core-collapse supernova. It represents the final evolutionary phase of a high mass star. ...
... speed of light. The light from the supernova, although a mere 1% or so of its total energy, nonetheless may be enough to outshine its entire galaxy for a period of days or weeks. This is a core-collapse supernova. It represents the final evolutionary phase of a high mass star. ...
Components of the Milky Way
... From our vantage - out in the disk, easiest to see the structure in the Milky Way in the infra-red. ...
... From our vantage - out in the disk, easiest to see the structure in the Milky Way in the infra-red. ...
The_Origin_of_the_Universe
... Computer models that reverse the expansion, lead to the idea that at one time the universe was a concentrated object of incredible mass and density that exploded. This theory of the origin of the universe is known as the “Big Bang Theory” Scientists currently believe the universe is about 10 to ...
... Computer models that reverse the expansion, lead to the idea that at one time the universe was a concentrated object of incredible mass and density that exploded. This theory of the origin of the universe is known as the “Big Bang Theory” Scientists currently believe the universe is about 10 to ...
Ivelina Sotirova Major: Biochemistry Senior at CUNY Hunter College
... The Accelerating Universe The discovery of this year’s Physics Nobel Prize Laureates challenged many concepts in the field of astronomy as it revealed a secret our Universe had been keeping for billions of years. The Supernova Cosmology Project (SCP) led by Saul Perlmutter, and the High-z Supernova ...
... The Accelerating Universe The discovery of this year’s Physics Nobel Prize Laureates challenged many concepts in the field of astronomy as it revealed a secret our Universe had been keeping for billions of years. The Supernova Cosmology Project (SCP) led by Saul Perlmutter, and the High-z Supernova ...
here - Tenafly Middle School
... • If something— including light—crosses the event horizon, it will be pulled into the black hole. ...
... • If something— including light—crosses the event horizon, it will be pulled into the black hole. ...
The Cycle of Star Formation
... The stellar winds, radiation pressure, and the shocks from supernovae have one additional effect: they can compress the surrounding gas and trigger additional star formation! ...
... The stellar winds, radiation pressure, and the shocks from supernovae have one additional effect: they can compress the surrounding gas and trigger additional star formation! ...
CNO and F abundances in the barium star HD 123396
... of mass transfer via Roche Lobe overflow or stellar winds, and the low eccentricities arise from tidal circularization (Boffin & Jorissen 1988; Han et al. 1995; Karakas et al. 2000; Izzard et al. 2010). In this context, CNO elements, along with s-process elements, are key tracers of the nucleosynthesi ...
... of mass transfer via Roche Lobe overflow or stellar winds, and the low eccentricities arise from tidal circularization (Boffin & Jorissen 1988; Han et al. 1995; Karakas et al. 2000; Izzard et al. 2010). In this context, CNO elements, along with s-process elements, are key tracers of the nucleosynthesi ...
Fluorine abundances in dwarf stars of the solar neighbourhood⋆
... in closer agreement with the most recent theoretical nucleosynthesis predicions (Cristallo et al. 2009), although they have a different dependence on the stellar metallicity. However, Lucatello et al. (2011) measured the F abundance of ten Galactic extrinsic carbon-rich, low-metallicity stars conclu ...
... in closer agreement with the most recent theoretical nucleosynthesis predicions (Cristallo et al. 2009), although they have a different dependence on the stellar metallicity. However, Lucatello et al. (2011) measured the F abundance of ten Galactic extrinsic carbon-rich, low-metallicity stars conclu ...
T Tauri Variable Type Star
... Pre Main Sequence – young, low mass stars that are contracting as they evolve toward their main sequence stage. Mostly made of Hydrogen, some Helium, and some trace elements. Of the trace elements, Lithium appears which is an indicator of stellar youth. Often have large protoplanetary accretion disk ...
... Pre Main Sequence – young, low mass stars that are contracting as they evolve toward their main sequence stage. Mostly made of Hydrogen, some Helium, and some trace elements. Of the trace elements, Lithium appears which is an indicator of stellar youth. Often have large protoplanetary accretion disk ...
Proton spectra
... Proton chemical shifts generally run from 0 to 12 ppm and are referenced from tetramethylsilane (TMS, (CH3)4Si). The lower chemical shifts are associated with protons that have a high electron density and are in what is known as the high field region. ...
... Proton chemical shifts generally run from 0 to 12 ppm and are referenced from tetramethylsilane (TMS, (CH3)4Si). The lower chemical shifts are associated with protons that have a high electron density and are in what is known as the high field region. ...
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.