lec-life-main-sequen..
... nucleus, two positrons, two gamma rays and two neutrinos, with two left-over protons which fly off to start p-p fusion over again elsewhere. 61H+ 4He++ + 21H+ + 2e+ + 2 + 2n [By the way, the positrons don’t just sit there. They fly off and combine with electrons, but that’s another story.] ...
... nucleus, two positrons, two gamma rays and two neutrinos, with two left-over protons which fly off to start p-p fusion over again elsewhere. 61H+ 4He++ + 21H+ + 2e+ + 2 + 2n [By the way, the positrons don’t just sit there. They fly off and combine with electrons, but that’s another story.] ...
Some observed properties of Dark Matter: a progress report on an
... • How do planetary systems form? • To date many planets have been detected indirectly • Direct detection: – Mass, radius, temperature, composition – ELT will provide large samples of mature giant planets in reflected light – Earth-like planets may be within reach ...
... • How do planetary systems form? • To date many planets have been detected indirectly • Direct detection: – Mass, radius, temperature, composition – ELT will provide large samples of mature giant planets in reflected light – Earth-like planets may be within reach ...
Fill in the blanks of each frame using the list of missing words given
... The fusing of two atoms is called nuclear fusion. Sometimes this is called hydrogen burning, but it isn’t burning as we know it. ...
... The fusing of two atoms is called nuclear fusion. Sometimes this is called hydrogen burning, but it isn’t burning as we know it. ...
Document
... Pulsations in a star Pulsation period and amplitude depend on the average density. P 1/2 [P=(4π/3G)1/2] Low density long P, high amplitude High density short P, low amplitude Density profile decides how deep the pulsations penetrate in the star. (Deeper the penetration ...
... Pulsations in a star Pulsation period and amplitude depend on the average density. P 1/2 [P=(4π/3G)1/2] Low density long P, high amplitude High density short P, low amplitude Density profile decides how deep the pulsations penetrate in the star. (Deeper the penetration ...
m 1
... m1 + m2 = (42 / GP2)P3(K1+K2)3/83sin3i = P(K1+K2)3/2G sin3i (m1+ m2)P2 = (a1+ a2)3 = a13(1+ a2/a1)3 ...
... m1 + m2 = (42 / GP2)P3(K1+K2)3/83sin3i = P(K1+K2)3/2G sin3i (m1+ m2)P2 = (a1+ a2)3 = a13(1+ a2/a1)3 ...
Article 8
... occurs.... nuclear fusion begins and the ball of gas and dust starts to glow. A new star has begun its life in our Universe. So what is this magical thing called "nuclear fusion" and why does it start happening inside the ball of gas and dust? It happens like this..... As the contraction of the gas ...
... occurs.... nuclear fusion begins and the ball of gas and dust starts to glow. A new star has begun its life in our Universe. So what is this magical thing called "nuclear fusion" and why does it start happening inside the ball of gas and dust? It happens like this..... As the contraction of the gas ...
The Structure of White Dwarf and Neutron Stars∗ Abstract
... This module is an introduction to the physics of white dwarfs and neutron stars, remnants left behind by ordinary stars after they have ceased nuclear fusion. These objects support themselves against gravitational collapse by physical mechanisms other than the pressure of hot gas (the heat being gen ...
... This module is an introduction to the physics of white dwarfs and neutron stars, remnants left behind by ordinary stars after they have ceased nuclear fusion. These objects support themselves against gravitational collapse by physical mechanisms other than the pressure of hot gas (the heat being gen ...
Sample Test 22
... using only hydrogen and helium. 3. Population II stars contain very little material in their atmospheres other than hydrogen and helium. They are old stars. Heavy elements do exist in their cores as byproducts of fusion reactions. 4. Population I stars contain heavier elements in their atmospheres. ...
... using only hydrogen and helium. 3. Population II stars contain very little material in their atmospheres other than hydrogen and helium. They are old stars. Heavy elements do exist in their cores as byproducts of fusion reactions. 4. Population I stars contain heavier elements in their atmospheres. ...
binary stars
... NB if the primary mass m1 can be obtained from the spectral type, the system can be solved. More generally the system will be inclined. If the radial velocity curve is sinusoidal, we know we are dealing with circular orbits in which case we measure the projected velocity Vr sini for each component. ...
... NB if the primary mass m1 can be obtained from the spectral type, the system can be solved. More generally the system will be inclined. If the radial velocity curve is sinusoidal, we know we are dealing with circular orbits in which case we measure the projected velocity Vr sini for each component. ...
The Sun and the Stars
... NB if the primary mass m1 can be obtained from the spectral type, the system can be solved. More generally the system will be inclined. If the radial velocity curve is sinusoidal, we know we are dealing with circular orbits in which case we measure the projected velocity Vr sini for each component. ...
... NB if the primary mass m1 can be obtained from the spectral type, the system can be solved. More generally the system will be inclined. If the radial velocity curve is sinusoidal, we know we are dealing with circular orbits in which case we measure the projected velocity Vr sini for each component. ...
Observational Data
... It is likely that the disk of the Milky Way has been formed by continuous accretion of gas from the reservoir, such as the Galactic halo and the IGM, but our simulation already takes into account cosmological gas infall. Our simulation does not take into account the effect of ionizing radiation fiel ...
... It is likely that the disk of the Milky Way has been formed by continuous accretion of gas from the reservoir, such as the Galactic halo and the IGM, but our simulation already takes into account cosmological gas infall. Our simulation does not take into account the effect of ionizing radiation fiel ...
arXiv:1604.01613v2 [astro-ph.SR] 23 Aug 2016
... SN Ia spectra (Branch et al. 1995). Moreover, there is both theoretical and observational evidence for a large population of close double white dwarf binaries (Yungelson et al. 1994; Nelemans & Tout 2005; Napiwotzki et al. 2001). However, there is some uncertainty as to whether the merger leads to a ...
... SN Ia spectra (Branch et al. 1995). Moreover, there is both theoretical and observational evidence for a large population of close double white dwarf binaries (Yungelson et al. 1994; Nelemans & Tout 2005; Napiwotzki et al. 2001). However, there is some uncertainty as to whether the merger leads to a ...
The white dwarf binary pathways survey – I. A sample of FGK stars
... SN Ia spectra (Branch et al. 1995). Moreover, there is both theoretical and observational evidence for a large population of close double white dwarf binaries (Yungelson et al. 1994; Nelemans & Tout 2005; Napiwotzki et al. 2001). However, there is some uncertainty as to whether the merger leads to a ...
... SN Ia spectra (Branch et al. 1995). Moreover, there is both theoretical and observational evidence for a large population of close double white dwarf binaries (Yungelson et al. 1994; Nelemans & Tout 2005; Napiwotzki et al. 2001). However, there is some uncertainty as to whether the merger leads to a ...
The correct answers are written in bold, italic and underlined. The
... Neutron stars have masses from 1.4 to 3 solar masses and are the collapsed cores of highmass stars. Low-mass stars end their lives as white dwarfs, not neutron stars. The maximum mass of a white dwarf is 1.4 solar masses, so even if a white dwarf explodes as a Type I supernova, it cannot form a neut ...
... Neutron stars have masses from 1.4 to 3 solar masses and are the collapsed cores of highmass stars. Low-mass stars end their lives as white dwarfs, not neutron stars. The maximum mass of a white dwarf is 1.4 solar masses, so even if a white dwarf explodes as a Type I supernova, it cannot form a neut ...
PPT Slides - Center for Computational Sciences
... • Densities build up until fusion starts in the center. ...
... • Densities build up until fusion starts in the center. ...
Xtra_credit_MC_chapt_10−12_2014.txt Xtra_credit_MC_chapt_10
... the star, helium starts to build up in the core and the video says: a) the star is on the "main sequence" b) fusion releases "a ton of energy" c) the core begins to shrink d) a) and b) e) a) and b) and c) 2) As helium builds up in the core of the star then the video says the core becomes: a) opaque ...
... the star, helium starts to build up in the core and the video says: a) the star is on the "main sequence" b) fusion releases "a ton of energy" c) the core begins to shrink d) a) and b) e) a) and b) and c) 2) As helium builds up in the core of the star then the video says the core becomes: a) opaque ...
Spots on Ap Stars
... • Chromospheric plasma heated to coronal temperatures, hot plasma flows up into the corona • Shock front moves downward to heat the photospheric base • As the density of the corona increases, it is further heated by the energetic electrons. Soft x-rays from the corona then heat the chromosphere ...
... • Chromospheric plasma heated to coronal temperatures, hot plasma flows up into the corona • Shock front moves downward to heat the photospheric base • As the density of the corona increases, it is further heated by the energetic electrons. Soft x-rays from the corona then heat the chromosphere ...
Summary of recent research activities
... (at that time no photometry had been published). Indeed new EFOSC2 spectra of its HII region yielded an oxygen abundance only slightly higher than that of I Zw 18 (Saviane et al. 2002), and our EMMI imaging revealed a well-defined RGB (Momany et al. 2002). However, the presence of carbon stars (Cook ...
... (at that time no photometry had been published). Indeed new EFOSC2 spectra of its HII region yielded an oxygen abundance only slightly higher than that of I Zw 18 (Saviane et al. 2002), and our EMMI imaging revealed a well-defined RGB (Momany et al. 2002). However, the presence of carbon stars (Cook ...
Models of rapidly rotating neutron stars: remnants of accretion
... suggesting that they are dynamically stable. Their analysis does not rule out the possibility that these models have non-axisymmetric secular instabilities, because the secular time-scale is expected to range from hundreds of milliseconds to a few minutes, much longer than their simulation time. The ...
... suggesting that they are dynamically stable. Their analysis does not rule out the possibility that these models have non-axisymmetric secular instabilities, because the secular time-scale is expected to range from hundreds of milliseconds to a few minutes, much longer than their simulation time. The ...
Astronomy 112: The Physics of Stars Class 17 Notes: Core Collapse
... Very massive stars, those above 85 M or so, lose mass in a rapid and unstable manner. We have already encountered one star like this: η Carinae. This is an example of a type of star called a luminous blue variable, or LBV. [Slide 1 – η Car] As these processes reduce the star’s mass, its atmosphere ...
... Very massive stars, those above 85 M or so, lose mass in a rapid and unstable manner. We have already encountered one star like this: η Carinae. This is an example of a type of star called a luminous blue variable, or LBV. [Slide 1 – η Car] As these processes reduce the star’s mass, its atmosphere ...
Weighing a galaxy / Black holes / Quasars —16 Nov Nov-09
... speed is greater than speed of light: nothing can escape. • If sun were squeezed to 3-km radius, light could not escape from it. • If Earth were squeezed to 1-cm radius, light could not escape from it. • Schwarzschild radius is boundary between inside & outside of a black hole. – Light can escape if ...
... speed is greater than speed of light: nothing can escape. • If sun were squeezed to 3-km radius, light could not escape from it. • If Earth were squeezed to 1-cm radius, light could not escape from it. • Schwarzschild radius is boundary between inside & outside of a black hole. – Light can escape if ...
the 82nd arthur h. compton lecture series
... of low-mass, there are a lot of binary systems composed of two stars with slightly different masses, yet still “low-mass”. ...
... of low-mass, there are a lot of binary systems composed of two stars with slightly different masses, yet still “low-mass”. ...
Subrahmanyan Chandrasekhar
... The Chandrasekhar Limit and the Fate of Stars In the years 1929 to 1939, when he was aged 18 to 28, Chandrasekhar was intensely interested in the physics of stars – astrophysics. Traveling by ship in 1930 to begin his Ph.D. at Cambridge University, he had calculated a number. In his honor this numbe ...
... The Chandrasekhar Limit and the Fate of Stars In the years 1929 to 1939, when he was aged 18 to 28, Chandrasekhar was intensely interested in the physics of stars – astrophysics. Traveling by ship in 1930 to begin his Ph.D. at Cambridge University, he had calculated a number. In his honor this numbe ...
The lifes of a star
... permanently. The reason is that Iron is a very stable nucleus so that if two Iron nuclei are slammed together they will only stick if energy is supplied (in contrast, two Hydrogen atoms stick and also release energy). When nuclear reactions stop gravitational contraction continues again and will pro ...
... permanently. The reason is that Iron is a very stable nucleus so that if two Iron nuclei are slammed together they will only stick if energy is supplied (in contrast, two Hydrogen atoms stick and also release energy). When nuclear reactions stop gravitational contraction continues again and will pro ...
SN 2004dj
... Supernovae might be the brightest objects in the universe, and can outshine a whole galaxy (for a few weeks) ...
... Supernovae might be the brightest objects in the universe, and can outshine a whole galaxy (for a few weeks) ...