(HR) diagram - Cloudfront.net
... calculate it based on other observations. It can be determined either by the inertial properties of the body or by its gravitational influence on other bodies. The larger the mass, the stronger the gravitational effect on the bodies around it. Stellar masses are expressed as multiples of the mass of ...
... calculate it based on other observations. It can be determined either by the inertial properties of the body or by its gravitational influence on other bodies. The larger the mass, the stronger the gravitational effect on the bodies around it. Stellar masses are expressed as multiples of the mass of ...
Document
... In context… Imagine each star in the Milky Way is the size of pea The 200 billion stars in the Galaxy would be a cube of peas 34m aside Scaling to the Milky Way, the typical distance between peas is 220km The Milky Way would stretch between the Earth and the Moon ...
... In context… Imagine each star in the Milky Way is the size of pea The 200 billion stars in the Galaxy would be a cube of peas 34m aside Scaling to the Milky Way, the typical distance between peas is 220km The Milky Way would stretch between the Earth and the Moon ...
F03HW12
... RQ 6: How can star clusters confirm our theories of stellar evolution? Answer: Star clusters contain stars of a wide variety of masses that all formed at about the same time. Since our models tell us that massive stars should evolve faster than low mass stars, we expect to see differences in the sta ...
... RQ 6: How can star clusters confirm our theories of stellar evolution? Answer: Star clusters contain stars of a wide variety of masses that all formed at about the same time. Since our models tell us that massive stars should evolve faster than low mass stars, we expect to see differences in the sta ...
Document
... What causes density waves? Smaller perturbations can be induced in galactic disks via interactions with other systems These grow to become pronounced waves. Seen in all kings of disks, including protostellar disks! ...
... What causes density waves? Smaller perturbations can be induced in galactic disks via interactions with other systems These grow to become pronounced waves. Seen in all kings of disks, including protostellar disks! ...
Red Supergiants as the Progenitors of Type IIP Supernova
... and while extending into the helium shell, fragment into ballistically moving clumps and filaments that propagate faster than the expansion of their environment. While for a 2D model with explosion energy around 1.8× 1051 erg the Si and Ni containing structures still move with nearly 4000 km s-1 (oxy ...
... and while extending into the helium shell, fragment into ballistically moving clumps and filaments that propagate faster than the expansion of their environment. While for a 2D model with explosion energy around 1.8× 1051 erg the Si and Ni containing structures still move with nearly 4000 km s-1 (oxy ...
stellar interiors instructor notes
... 10. The Interiors of Stars Goals: 1. Develop the basic equations describing equilibrium conditions applying in stellar interiors. 2. Estimate the physical conditions that must exist at the centre of a typical star, the Sun. 3. Outline potential sources of energy generation in stars and investigate t ...
... 10. The Interiors of Stars Goals: 1. Develop the basic equations describing equilibrium conditions applying in stellar interiors. 2. Estimate the physical conditions that must exist at the centre of a typical star, the Sun. 3. Outline potential sources of energy generation in stars and investigate t ...
Review for Astronomy 3 Midterm #2
... are hydrogen poor (since white dwarfs are mostly made of carbon), and their light curves will be different. Type II Supernovae occur when the high mass stars described above undergo iron core collapse. The outer layers will hit the core like they are running into a “brick wall” and the shock wave ...
... are hydrogen poor (since white dwarfs are mostly made of carbon), and their light curves will be different. Type II Supernovae occur when the high mass stars described above undergo iron core collapse. The outer layers will hit the core like they are running into a “brick wall” and the shock wave ...
Stellar Evolution
... Carbon to burn. Nevertheless, the total energy output is increasing, which causes the star to puff up again, the surface temperature to decrease and to appear redder. The star is again a Red Giant on its way of turning into a Supergiant. Red giants and supergiants can have strong “winds” that dispel ...
... Carbon to burn. Nevertheless, the total energy output is increasing, which causes the star to puff up again, the surface temperature to decrease and to appear redder. The star is again a Red Giant on its way of turning into a Supergiant. Red giants and supergiants can have strong “winds” that dispel ...
The Death of Massive Stars
... 100 solar masses will emit radiation so intense that it will prevent more material from falling into the star, thereby limiting the star’s size. • Lower limit of Star’s Mass: Protostars with masses of less than 0.08 solar masses do not have enough internal pressure to ignite hydrogen fusion. – What ...
... 100 solar masses will emit radiation so intense that it will prevent more material from falling into the star, thereby limiting the star’s size. • Lower limit of Star’s Mass: Protostars with masses of less than 0.08 solar masses do not have enough internal pressure to ignite hydrogen fusion. – What ...
Boron is the chemical element with atomic number 5 and
... phases are based on B12 icosahedra, the γ‐phase can be described as a rocksalt‐type arrangement of the icosahedra and B2 atomic pairs.[21] It can be produced by compressing other boron phases to 12–20 GPa and heating to 1500–1800 °C; it remains stable after releasing the temperature and pressure. ...
... phases are based on B12 icosahedra, the γ‐phase can be described as a rocksalt‐type arrangement of the icosahedra and B2 atomic pairs.[21] It can be produced by compressing other boron phases to 12–20 GPa and heating to 1500–1800 °C; it remains stable after releasing the temperature and pressure. ...
Unit 8 Chapter 30 Stars, Galaxies and the Universe
... metals (U, Pb, Fe, Ni). When all of the fuel is used up the collapse of these metals is very rapid. The star can not contain all the material, it just EXPLODES. The death takes millions of years, but when it gets to the core, it can take a few weeks to a few months. This becomes the source material ...
... metals (U, Pb, Fe, Ni). When all of the fuel is used up the collapse of these metals is very rapid. The star can not contain all the material, it just EXPLODES. The death takes millions of years, but when it gets to the core, it can take a few weeks to a few months. This becomes the source material ...
vuorinen_neutron_stars
... Main reference: Kurkela, Fraga, Schaffner-Bielich, AV, ApJ 789 (1402.6618) ...
... Main reference: Kurkela, Fraga, Schaffner-Bielich, AV, ApJ 789 (1402.6618) ...
powerpoint file - QUB Astrophysics Research Centre
... central part of the curve (corresponding to close to a solar mass) is approximated by a power law, it has an exponent of approximately 5. Which is in good agreement with the value of 5.46 above. Similarly the lower part of the main-sequence on the observed L-Te diagram (HR diagram) is well represent ...
... central part of the curve (corresponding to close to a solar mass) is approximated by a power law, it has an exponent of approximately 5. Which is in good agreement with the value of 5.46 above. Similarly the lower part of the main-sequence on the observed L-Te diagram (HR diagram) is well represent ...
Looking back in time to the big bang theory activity
... ICT, English skills, and presentation skills. You can also link this work to how science works. The redshift analysis task gives learners an opportunity to relate what they have learned to a real life scenario. The evidence for the Big Bang task gives learners an opportunity to voice their opinions ...
... ICT, English skills, and presentation skills. You can also link this work to how science works. The redshift analysis task gives learners an opportunity to relate what they have learned to a real life scenario. The evidence for the Big Bang task gives learners an opportunity to voice their opinions ...
Misc-ReviewForAstroTest
... Sun expands orbit of Venus or Earth Star 8 solar masses -> 1 or 2 residual ...
... Sun expands orbit of Venus or Earth Star 8 solar masses -> 1 or 2 residual ...
ASTRONOMY AND ASTROPHYSICS Barium abundances in cool
... are nearly free of blends. As Ba II is the dominant ionization stage in such atmospheres and the observable lines arise from the ground state ( s) or the low-excited d term (with the excitation energy of : eV) these Ba II lines can be detected even in extremely metal-poor stars. Two types of neutr ...
... are nearly free of blends. As Ba II is the dominant ionization stage in such atmospheres and the observable lines arise from the ground state ( s) or the low-excited d term (with the excitation energy of : eV) these Ba II lines can be detected even in extremely metal-poor stars. Two types of neutr ...
L7 - QUB Astrophysics Research Centre
... central part of the curve (corresponding to close to a solar mass) is approximated by a power law, it has an exponent of approximately 5. Which is in good agreement with the value of 5.46 above. Similarly the lower part of the main-sequence on the observed L-Te diagram (HR diagram) is well represent ...
... central part of the curve (corresponding to close to a solar mass) is approximated by a power law, it has an exponent of approximately 5. Which is in good agreement with the value of 5.46 above. Similarly the lower part of the main-sequence on the observed L-Te diagram (HR diagram) is well represent ...
doc - IAC
... the signature of the element’s formation, which gives us a better idea of the nucleosynthesis in all those stars.’ But planetary nebulae harbour much more information. ‘For example,’ the researcher continues, ‘these objects have emission lines, although very few, for which reason they are very easy ...
... the signature of the element’s formation, which gives us a better idea of the nucleosynthesis in all those stars.’ But planetary nebulae harbour much more information. ‘For example,’ the researcher continues, ‘these objects have emission lines, although very few, for which reason they are very easy ...
Primas
... A cool, thin gas seen in front of a hot source produces absorpDon lines: in the conDnuum region, τ is low and we see primarily the background source. At the wavelengths of spectral lines, τ is ...
... A cool, thin gas seen in front of a hot source produces absorpDon lines: in the conDnuum region, τ is low and we see primarily the background source. At the wavelengths of spectral lines, τ is ...
Sporadic Mass Ejection in Red Supergiants
... correlation among these three quantities would support the model developed here. An increasingly large body of observational evidence now supports the theory that mass expulsion in late type stars is driven by large-scale shock waves in extended cool atmospheres. Willson (1976) has suggested that st ...
... correlation among these three quantities would support the model developed here. An increasingly large body of observational evidence now supports the theory that mass expulsion in late type stars is driven by large-scale shock waves in extended cool atmospheres. Willson (1976) has suggested that st ...
File
... You have learned that each group of the periodic table has similar properties. For example, the metals of Group 1 are so reactive they don’t exist uncombined in nature. The Group 2 metals are also quite reactive. The table below shows atomic radius and reactivity of most of the metals in Groups 1 an ...
... You have learned that each group of the periodic table has similar properties. For example, the metals of Group 1 are so reactive they don’t exist uncombined in nature. The Group 2 metals are also quite reactive. The table below shows atomic radius and reactivity of most of the metals in Groups 1 an ...
galaxy phenomenology
... SDSS images of spiral galaxies, selected according to classifications in NED to be Sa–Sd (including barred types). The images are sorted by absolute magnitude in the horizontal direction, ranging between Mr − 5 log10 h ∼ −18.5 and −22 from left to right, and g − r color in the vertical direction, ra ...
... SDSS images of spiral galaxies, selected according to classifications in NED to be Sa–Sd (including barred types). The images are sorted by absolute magnitude in the horizontal direction, ranging between Mr − 5 log10 h ∼ −18.5 and −22 from left to right, and g − r color in the vertical direction, ra ...
Astronomy 535 Stellar Structure Evolution
... “Crush them, crush them all!” -Professor John Feldmeier ...
... “Crush them, crush them all!” -Professor John Feldmeier ...
Lecture 13 Hydrogen Burning on the Main Sequence and Homology
... (or protostar) in hydrostatic equilibrium contracts its central temperature rises as the cube root of the density. It also says that stars (or protostars) will have a higher temperature at a given density if their mass is bigger. In the absence of nuclear reactions the contraction occurs at a rate n ...
... (or protostar) in hydrostatic equilibrium contracts its central temperature rises as the cube root of the density. It also says that stars (or protostars) will have a higher temperature at a given density if their mass is bigger. In the absence of nuclear reactions the contraction occurs at a rate n ...
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.