Star Classification
... At extremely high temperatures the coil will turn yellow-white, or even blue-white (it’s hard to imagine a stove coil getting that hot). A star’s color is also determined by the temperature of the star’s surface. Relatively cool stars are red, warmer stars are orange or yellow, and extremely hot sta ...
... At extremely high temperatures the coil will turn yellow-white, or even blue-white (it’s hard to imagine a stove coil getting that hot). A star’s color is also determined by the temperature of the star’s surface. Relatively cool stars are red, warmer stars are orange or yellow, and extremely hot sta ...
Interstellar Astrophysics Summary notes: Part 5
... the protostar by convection, warming its surface. As the radius of the protostar decreases, the luminosity decreases at almost constant surface (effective) temperature. On the H-R diagram this change in L at ∼constant T thus gives a nearly vertical track known as a convective Hayashi evolutionary tr ...
... the protostar by convection, warming its surface. As the radius of the protostar decreases, the luminosity decreases at almost constant surface (effective) temperature. On the H-R diagram this change in L at ∼constant T thus gives a nearly vertical track known as a convective Hayashi evolutionary tr ...
Lecture 6-1: Schematic Evolution of Stars as seen from the core
... pressure scales with r while hydrostatic pressure scales with r4/3, a more massive star requires a higher central temperature (and/or lower density). For a non-relativistic degenerate gas, temperature doesn’t enter. Now, thermal pressure scales with r5/3 while hydrostatic pressure scales with r4/3, ...
... pressure scales with r while hydrostatic pressure scales with r4/3, a more massive star requires a higher central temperature (and/or lower density). For a non-relativistic degenerate gas, temperature doesn’t enter. Now, thermal pressure scales with r5/3 while hydrostatic pressure scales with r4/3, ...
Unit 1
... – Most have surface temperatures of ~5000K, so appear yellow – Most are giants (Yellow Giants) – Instability comes from partial absorption of radiation in the interior of the star • Helium absorbs radiation, and the outer layers of the star get pushed away from core • As the star expands, the densit ...
... – Most have surface temperatures of ~5000K, so appear yellow – Most are giants (Yellow Giants) – Instability comes from partial absorption of radiation in the interior of the star • Helium absorbs radiation, and the outer layers of the star get pushed away from core • As the star expands, the densit ...
File - Morgan, Kristen
... These astronomers believe 18-20 billion years ago all of the matter in the universe was packed into a very dense, very hot spot smaller than a dot! ...
... These astronomers believe 18-20 billion years ago all of the matter in the universe was packed into a very dense, very hot spot smaller than a dot! ...
Star Types - University of Massachusetts Amherst
... Star A is closer than Star B Star B is closer than Star A The stars are at the same distance Not enough information is given ...
... Star A is closer than Star B Star B is closer than Star A The stars are at the same distance Not enough information is given ...
1. The distances to the most remote galaxies can be
... a) have all their stars on the main sequence. b) Have only their high mass stars on the main sequence while the low-mass protostars are still contracting (and hence are not on the main sequence yet). c) Have only their low mass stars on the main sequence while the high-mass protostars are still cont ...
... a) have all their stars on the main sequence. b) Have only their high mass stars on the main sequence while the low-mass protostars are still contracting (and hence are not on the main sequence yet). c) Have only their low mass stars on the main sequence while the high-mass protostars are still cont ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... The surface luminosity of the sun is L =3.86x1026W, and at no point in the Sun can the luminosity exceed this value (see eqn of energy production). What can you conclude from this ? As the T and v of the rising elements are determined by the difference between the actual temperature gradient and a ...
... The surface luminosity of the sun is L =3.86x1026W, and at no point in the Sun can the luminosity exceed this value (see eqn of energy production). What can you conclude from this ? As the T and v of the rising elements are determined by the difference between the actual temperature gradient and a ...
r - QUB Astrophysics Research Centre
... The surface luminosity of the sun is L =3.86x1026W, and at no point in the Sun can the luminosity exceed this value (see eqn of energy production). What can you conclude from this ? As the T and v of the rising elements are determined by the difference between the actual temperature gradient and a ...
... The surface luminosity of the sun is L =3.86x1026W, and at no point in the Sun can the luminosity exceed this value (see eqn of energy production). What can you conclude from this ? As the T and v of the rising elements are determined by the difference between the actual temperature gradient and a ...
Chapter 30 Graphing skills worksheet
... Line Graphs and the Surface Temperature of Stars Astronomers can determine the temperature of individual stars based on their color. The temperature of the star is higher as you move across the spectrum from red to blue. The data that shows this is found in the table below. Surface Temperature of St ...
... Line Graphs and the Surface Temperature of Stars Astronomers can determine the temperature of individual stars based on their color. The temperature of the star is higher as you move across the spectrum from red to blue. The data that shows this is found in the table below. Surface Temperature of St ...
Lesson 2 | The Sun and Other Stars
... 3. elements, including helium and hydrogen gas, that make up a star ...
... 3. elements, including helium and hydrogen gas, that make up a star ...
Slide 1 - cosmos.esa.int
... Formation scenarios – If we form them, they will form BHs. Stellar evolution: current issues Issues in collapse Neutrinos from Massive Stars ...
... Formation scenarios – If we form them, they will form BHs. Stellar evolution: current issues Issues in collapse Neutrinos from Massive Stars ...
ppt
... How do the photons ever get out? Temperature of star decreases outward from center. This causes the radiation pressure to decrease outwards as well ...
... How do the photons ever get out? Temperature of star decreases outward from center. This causes the radiation pressure to decrease outwards as well ...
bright - TutorPlus
... depending on their position on the H-R diagram. • Most stars line up along a slightly curved diagonal line called the main sequence. Our Sun is located on the main sequence. • On the main sequence, low mass stars tend to be cooler and less bright whereas high mass stars are hotter, brighter and loca ...
... depending on their position on the H-R diagram. • Most stars line up along a slightly curved diagonal line called the main sequence. Our Sun is located on the main sequence. • On the main sequence, low mass stars tend to be cooler and less bright whereas high mass stars are hotter, brighter and loca ...
Photosphere
... flux, the amount of energy we on Earth receive per second per area of telescope. • Reasoning process: • If the temperature is hotter, the flux is ___ (greater or less). ...
... flux, the amount of energy we on Earth receive per second per area of telescope. • Reasoning process: • If the temperature is hotter, the flux is ___ (greater or less). ...
The structure and evolution of stars
... we will derive an expression relating the change in temperature with radius in a star assuming all energy is transported by radiation. Hence we ignore the effects of convection and conduction. We will make use of your knowledge of Marianne Faurobert, which covered stellar atmospheres and radiative t ...
... we will derive an expression relating the change in temperature with radius in a star assuming all energy is transported by radiation. Hence we ignore the effects of convection and conduction. We will make use of your knowledge of Marianne Faurobert, which covered stellar atmospheres and radiative t ...
Stellar Evolution and the HR Diagram – Study Guide
... 13. White dwarfs are about the size of __Earth (planets)__ . 14. Neutron stars are about ___12__ miles in diameter. 15. Our Sun is a G2___ class star. 16. The MOST massive of stars live (the longest or the shortest) lives. 17. Supernovas are produced by the explosion of _super massive__ stars. The r ...
... 13. White dwarfs are about the size of __Earth (planets)__ . 14. Neutron stars are about ___12__ miles in diameter. 15. Our Sun is a G2___ class star. 16. The MOST massive of stars live (the longest or the shortest) lives. 17. Supernovas are produced by the explosion of _super massive__ stars. The r ...
Activity: Stellar Spectra
... 5. Using the spectra given try to identify the mystery star at the bottom of the page. Click on the boxes for the elements you think are present then click ‘Did I get it Right?’ 6. If you got it right record the elements present in your observations table, then click on ‘Give me another star’ and tr ...
... 5. Using the spectra given try to identify the mystery star at the bottom of the page. Click on the boxes for the elements you think are present then click ‘Did I get it Right?’ 6. If you got it right record the elements present in your observations table, then click on ‘Give me another star’ and tr ...
giant molecular clouds
... Imagine a star’s interior composed of individual shells. Within each shell, two forces have to be in equilibrium with each other: Gravity, i.e. the weight from all layers above ...
... Imagine a star’s interior composed of individual shells. Within each shell, two forces have to be in equilibrium with each other: Gravity, i.e. the weight from all layers above ...
Lecture 12
... L = 4pR 2 ¥ sTe4 …which relates L, R and Te - so only three independent quantities to measure - mass plus two of luminosity, radius, and effective temperature. ...
... L = 4pR 2 ¥ sTe4 …which relates L, R and Te - so only three independent quantities to measure - mass plus two of luminosity, radius, and effective temperature. ...
Lecture 5/10 The interstellar medium and star formation Ulf
... radiation ionises the surrounding hydrogen gas and we get HII regions. In these regions there is a balance between the ionisation of neutral hydrogen atoms by the ultraviolet photons and the recombination of protons and electrons. During the recombination events the electrons cascade down through th ...
... radiation ionises the surrounding hydrogen gas and we get HII regions. In these regions there is a balance between the ionisation of neutral hydrogen atoms by the ultraviolet photons and the recombination of protons and electrons. During the recombination events the electrons cascade down through th ...
fall semester review
... 41. What does volume measure?The amount of space matter takes up 42. Susan goes on a trip and packs 3 shirts and 3 pairs of jeans in her suitcase. On her trip she purchased 4 souvenir t-shirts and a sweatshirt. When she was leaving her hotel, she had to stuff all of these items into the same suitcas ...
... 41. What does volume measure?The amount of space matter takes up 42. Susan goes on a trip and packs 3 shirts and 3 pairs of jeans in her suitcase. On her trip she purchased 4 souvenir t-shirts and a sweatshirt. When she was leaving her hotel, she had to stuff all of these items into the same suitcas ...
Ch. 11 and 12 Study Guide (ANSWERS)
... 15) What is a nebula (pg. 519)? A nebula is a cloud of dust and gas in space. 16) The elements, hydrogen and helium, are the most common in nebulae. 17) What is nuclear fusion? Nuclear fusion is a reaction in which 2 atomic nuclei combine to form a large nucleus with a higher mass. Energy is release ...
... 15) What is a nebula (pg. 519)? A nebula is a cloud of dust and gas in space. 16) The elements, hydrogen and helium, are the most common in nebulae. 17) What is nuclear fusion? Nuclear fusion is a reaction in which 2 atomic nuclei combine to form a large nucleus with a higher mass. Energy is release ...