Integrative Studies 410 Our Place in the Universe
... – Luminosity about 1000 times that of the sun – Duration ~ 1 million years – Temperature ~ 1 million K at core, 3,000 K at surface • Still too cool for nuclear ...
... – Luminosity about 1000 times that of the sun – Duration ~ 1 million years – Temperature ~ 1 million K at core, 3,000 K at surface • Still too cool for nuclear ...
Document
... luminosity L=10-2LSun and an effective temperature Teff=3,200 K. What is the approximate density of this M dwarf? • Calculate the effective temperature of a protostellar object with a luminosity 50 times greater than the Sun and a diameter of 3” at a distance of ...
... luminosity L=10-2LSun and an effective temperature Teff=3,200 K. What is the approximate density of this M dwarf? • Calculate the effective temperature of a protostellar object with a luminosity 50 times greater than the Sun and a diameter of 3” at a distance of ...
Life Cycle of a Star - Intervention Worksheet
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
Stars Life Cycle WS
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
Stellar Evolution Reading Questions Integrated Science 2 Name
... 3. Most stars go through the same three stages before they die. Describe each stage below. Include how long it lasts, what the main events are, and what causes it to move to the next stage. ...
... 3. Most stars go through the same three stages before they die. Describe each stage below. Include how long it lasts, what the main events are, and what causes it to move to the next stage. ...
Slide 1
... density ~ 10 million g/cc, and ignites Neon burning to Mg and Si; lasts only a few years - Oxygen shell burns up to Si, S, P…(Si-core) ...
... density ~ 10 million g/cc, and ignites Neon burning to Mg and Si; lasts only a few years - Oxygen shell burns up to Si, S, P…(Si-core) ...
Star- large ball of gas held together by large ball of gas held
... Stars originate from clouds of gas and dust molecules that clump up due to gravity. When the clump reaches the size of Jupiter, it creates enough energy by nuclear fusion to shine – becoming a star. For stars that are about the size of our sun, after main sequence they become giants, white dwarfs, a ...
... Stars originate from clouds of gas and dust molecules that clump up due to gravity. When the clump reaches the size of Jupiter, it creates enough energy by nuclear fusion to shine – becoming a star. For stars that are about the size of our sun, after main sequence they become giants, white dwarfs, a ...
DTU9ePPTChap13 - Faculty Lounge : Astronomy
... transition from the main sequence to the giant phase. The asterisk (*) shows the helium flash occurring in a low-mass star. (b) After the helium flash, the star converts its helium core into carbon and oxygen. While doing so, its core reexpands, decreasing shell fusion. As a result, the star’s outer ...
... transition from the main sequence to the giant phase. The asterisk (*) shows the helium flash occurring in a low-mass star. (b) After the helium flash, the star converts its helium core into carbon and oxygen. While doing so, its core reexpands, decreasing shell fusion. As a result, the star’s outer ...
Light n-Capture Element Abundances in Metal
... processes; some are well known, others are still the object of active research. The elements Zirconium (Zr) and Yttrium (Y) are produced via neutron capture (ncapture). These elements reside in the mass range where there is uncertainty about the production mechanism at early time. The rapid n-captur ...
... processes; some are well known, others are still the object of active research. The elements Zirconium (Zr) and Yttrium (Y) are produced via neutron capture (ncapture). These elements reside in the mass range where there is uncertainty about the production mechanism at early time. The rapid n-captur ...
Lect16-3-28-and-30-1..
... of the core, act as catalysts for hydrogen fusion into helium. That is, the concentrations of C, N, and O are left unchanged by the fusion reactions, but they permit hydrogen to fuse into helium through a chain of reactions, called the CNO cycle, that makes the helium production rate far higher than ...
... of the core, act as catalysts for hydrogen fusion into helium. That is, the concentrations of C, N, and O are left unchanged by the fusion reactions, but they permit hydrogen to fuse into helium through a chain of reactions, called the CNO cycle, that makes the helium production rate far higher than ...
Introduction: The Night Sky
... form neutrons in extreme cases even this may not be stable, and a black hole is formed instead ...
... form neutrons in extreme cases even this may not be stable, and a black hole is formed instead ...
White Dwarfs
... some observed properties of type Ia and type II supernovae? a. Type Ia supernovae have hydrogen lines in their spectra. b. Type II supernovae have hydrogen lines in their spectra. c. Type Ia supernovae are more luminous. d. Both a and c above. e. Both b and c above. ...
... some observed properties of type Ia and type II supernovae? a. Type Ia supernovae have hydrogen lines in their spectra. b. Type II supernovae have hydrogen lines in their spectra. c. Type Ia supernovae are more luminous. d. Both a and c above. e. Both b and c above. ...
u = ′ u +V 1+ V ′ u c2 = 0.99c + 0.9999c 1+(0.99× 0.9999
... Boston area. How much mass would have to be converted to energy in order to supply that electrical power? A typical electric bill for a family is the order of $100 per month. At $0.10 per KiloWatt hour that is 1000 KWh. (As usual with these kinds of estimations, order of magnitude is what is aimed f ...
... Boston area. How much mass would have to be converted to energy in order to supply that electrical power? A typical electric bill for a family is the order of $100 per month. At $0.10 per KiloWatt hour that is 1000 KWh. (As usual with these kinds of estimations, order of magnitude is what is aimed f ...
Neutron stars and black holes
... explosion of a star more massive than 8 solar masses. Recall that a Type II supernova is the explosion of a single, massive star. Type Ib and Ic supernovae are also explosions of single, massive stars, but stars which have lost their outer envelopes of hydrogen or hydrogen and helium. A pulsar does ...
... explosion of a star more massive than 8 solar masses. Recall that a Type II supernova is the explosion of a single, massive star. Type Ib and Ic supernovae are also explosions of single, massive stars, but stars which have lost their outer envelopes of hydrogen or hydrogen and helium. A pulsar does ...
earth & space science
... Some white dwarfs revolve around red giants. When this happens, the gravity of the whit dwarf may capture gases from the red giant. As these gases accumulate on the surface of the white dwarf, pressure begins to build up. This pressure may cause large explosions. These explosions are called novas. ...
... Some white dwarfs revolve around red giants. When this happens, the gravity of the whit dwarf may capture gases from the red giant. As these gases accumulate on the surface of the white dwarf, pressure begins to build up. This pressure may cause large explosions. These explosions are called novas. ...
DTU_9e_ch13
... transition from the main sequence to the giant phase. The asterisk (*) shows the helium flash occurring in a low-mass star. (b) After the helium flash, the star converts its helium core into carbon and oxygen. While doing so, its core reexpands, decreasing shell fusion. As a result, the star’s outer ...
... transition from the main sequence to the giant phase. The asterisk (*) shows the helium flash occurring in a low-mass star. (b) After the helium flash, the star converts its helium core into carbon and oxygen. While doing so, its core reexpands, decreasing shell fusion. As a result, the star’s outer ...
Pistol Star - University of Dayton
... •When hydrogen or helium fuse, energy is released. In contrast, iron fusion absorbs the energy and cools a star. When this happens the thermal pressure that forced the stellar gases outward diminishes , and the star collapses under the influence of gravity. •Due to this strange phenomena supernovas ...
... •When hydrogen or helium fuse, energy is released. In contrast, iron fusion absorbs the energy and cools a star. When this happens the thermal pressure that forced the stellar gases outward diminishes , and the star collapses under the influence of gravity. •Due to this strange phenomena supernovas ...
Nuclear Fusion – when two H atoms combine to form one atom thus
... Nebula – Stars are formed or “born” in a nebula. Massive cosmic cloud of matter from which stars are created. Light Year – distance light travels in one year. 186,000 miles/sec – speed of light Life Cycle of a Star Stars start off as a nebula until a nuclear explosion causes the star to shine. The n ...
... Nebula – Stars are formed or “born” in a nebula. Massive cosmic cloud of matter from which stars are created. Light Year – distance light travels in one year. 186,000 miles/sec – speed of light Life Cycle of a Star Stars start off as a nebula until a nuclear explosion causes the star to shine. The n ...
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.