![Stars Power Point](http://s1.studyres.com/store/data/008080492_1-e6d589d3003e85b08d0e093b54d9455f-300x300.png)
It is evident from our observations of impact craters on planets and
... The cause of auroras was explained and the connection to why they are more prominent near the poles was linked to Earth’s magnetic field. Understanding the stars has been greatly augmented with the development of large telescopes and instruments that accurately measure and analyze starlight. In part ...
... The cause of auroras was explained and the connection to why they are more prominent near the poles was linked to Earth’s magnetic field. Understanding the stars has been greatly augmented with the development of large telescopes and instruments that accurately measure and analyze starlight. In part ...
The Fate of Massive Stars
... increased opacity due to presence of various Ions (including Fe) in stellar atmosphere Diagonal upper-luminosity cutoff that is temperature dependent Hotter --> Higher Luminosity cutoff Greater mass-loss/stellar winds for cooler stars at lower luminosities Stellar winds important contribution to ISM ...
... increased opacity due to presence of various Ions (including Fe) in stellar atmosphere Diagonal upper-luminosity cutoff that is temperature dependent Hotter --> Higher Luminosity cutoff Greater mass-loss/stellar winds for cooler stars at lower luminosities Stellar winds important contribution to ISM ...
Document
... how far away it must be to look that faint. • For any star in the sky, we KNOW: – Apparent Magnitude (m) – Spectral Type (O, B, A, F, G, K, M) – Luminosity Class (Main Sequence, Giant, etc…). These are denoted by a roman numeral (V, III, I,…). ...
... how far away it must be to look that faint. • For any star in the sky, we KNOW: – Apparent Magnitude (m) – Spectral Type (O, B, A, F, G, K, M) – Luminosity Class (Main Sequence, Giant, etc…). These are denoted by a roman numeral (V, III, I,…). ...
Milky Way
... • From variable stars we know distances. • From Doppler shift we know rotation velocity. • Use Kepler’s Third Law (again) to get mass of the Milky Way. More than what we see. • M = 1011 x Msun ...
... • From variable stars we know distances. • From Doppler shift we know rotation velocity. • Use Kepler’s Third Law (again) to get mass of the Milky Way. More than what we see. • M = 1011 x Msun ...
ReviewQuestionsForClass
... How do size, temperature, and distance to a star affect its brightness? Which stars on the main sequence are the brightest? Hottest? Biggest? Bluest? Live the longest? What are the different astronomical objects? Comets, nebulae, main sequence stars, red giants, white dwarves, planetary nebulae, bin ...
... How do size, temperature, and distance to a star affect its brightness? Which stars on the main sequence are the brightest? Hottest? Biggest? Bluest? Live the longest? What are the different astronomical objects? Comets, nebulae, main sequence stars, red giants, white dwarves, planetary nebulae, bin ...
The Inverse Square Law and Surface Area
... Earth is called the intensity (I) of the star’s radiation This is related to the power output per metre squared L of the star’s surface in this way ...
... Earth is called the intensity (I) of the star’s radiation This is related to the power output per metre squared L of the star’s surface in this way ...
Chapter 8: Stars
... • The combination of their ideas is now called the Hertzsprung-Russell Diagram, or HR Diagram. • The HR Diagram is a graph that shows the relationship between a stars’ surface temperature and its absolute magnitude. • The modern HR Diagram is shown below. ...
... • The combination of their ideas is now called the Hertzsprung-Russell Diagram, or HR Diagram. • The HR Diagram is a graph that shows the relationship between a stars’ surface temperature and its absolute magnitude. • The modern HR Diagram is shown below. ...
Star Types
... The Hertzsprung-Russell Diagram The HR diagram separates The effects of temperature And surface area on stars’ Luminosity and sorts the Stars according to their size ...
... The Hertzsprung-Russell Diagram The HR diagram separates The effects of temperature And surface area on stars’ Luminosity and sorts the Stars according to their size ...
Stars and Universe Test Review - Garnet Valley School District
... 2. __________________________ hot, very dense, Earth-sized stars 3. __________________________ matter that does not give off electromagnetic radiation 4. __________________________ a telescope that uses lenses or mirrors to collect and focus visible light 5. __________________________ the apparent s ...
... 2. __________________________ hot, very dense, Earth-sized stars 3. __________________________ matter that does not give off electromagnetic radiation 4. __________________________ a telescope that uses lenses or mirrors to collect and focus visible light 5. __________________________ the apparent s ...
Formation of Stars - mcp
... 3. Our sun is used to determine masses of stars ◦ 1.0 solar mass = mass of our sun ◦ If a stellar object is less than .01 solar mass it will not turn into a star ...
... 3. Our sun is used to determine masses of stars ◦ 1.0 solar mass = mass of our sun ◦ If a stellar object is less than .01 solar mass it will not turn into a star ...
Astronomy Chapter 13 Name
... O. Two stars in orbit around each other, held together by their mutual gravity P. A pair of stars held together by their mutual gravity and in orbit about each other, and which can be seen with a telescope as separate objects ...
... O. Two stars in orbit around each other, held together by their mutual gravity P. A pair of stars held together by their mutual gravity and in orbit about each other, and which can be seen with a telescope as separate objects ...
STELLAR EVOLUTION
... fusing hydrogen quietly in their cores. Their surface temperature and luminosity change very little during this time. Stars then evolve, progressively burning the “ash” of one fusion process in the next fusion process, until they exhaust all fuel possibilities. The star then ends its existence as a ...
... fusing hydrogen quietly in their cores. Their surface temperature and luminosity change very little during this time. Stars then evolve, progressively burning the “ash” of one fusion process in the next fusion process, until they exhaust all fuel possibilities. The star then ends its existence as a ...
Size Color and Temperature
... than the Sun. If Betelgeuse replaced the Sun, it would fill space in our solar system well beyond Earth’s orbit. Because giant and supergiant stars have such huge surface areas to give off light, they are very bright. Betelgeuse is one of the brightest stars in the sky, even though it is 522 light-y ...
... than the Sun. If Betelgeuse replaced the Sun, it would fill space in our solar system well beyond Earth’s orbit. Because giant and supergiant stars have such huge surface areas to give off light, they are very bright. Betelgeuse is one of the brightest stars in the sky, even though it is 522 light-y ...
SES4U Life Cycle of a Star
... the protostar becomes a brown dwarf and never reaches star status If critical temperature is reached, nuclear fusion begins (H fuses into He for the first time) ...
... the protostar becomes a brown dwarf and never reaches star status If critical temperature is reached, nuclear fusion begins (H fuses into He for the first time) ...
Option: Astrophysics Objects in the Universe: Asteroid: a small rocky
... Clusters: gravitationally bound system of galaxies or stars o Stellar cluster: group of stars held together by gravitation in the same region of space, created roughly at the same time from the same nebulae o Open Cluster: Up to several hundred stars that are 10 billion years old or less. May still ...
... Clusters: gravitationally bound system of galaxies or stars o Stellar cluster: group of stars held together by gravitation in the same region of space, created roughly at the same time from the same nebulae o Open Cluster: Up to several hundred stars that are 10 billion years old or less. May still ...
Stars
... • Is a yellow star hotter or cooler than an orange star? • Suppose you see two stars of the same apparent magnitude. If one star is actually four times as far away as the other, how much brighter would the farther star really be? ...
... • Is a yellow star hotter or cooler than an orange star? • Suppose you see two stars of the same apparent magnitude. If one star is actually four times as far away as the other, how much brighter would the farther star really be? ...
Useful Things to Study (#2)
... Cause of the aurora borealis/australis in the Earth’s atmosphere ...
... Cause of the aurora borealis/australis in the Earth’s atmosphere ...
Hubble`s Law is the relation between the recession velocity of a
... Hubble's Law is the relation between the recession velocity of a galaxy and its distance: Vr = H d, that is, the velocity of recession Vr equals the distance d times the Hubble constant H. Assuming the galaxies have receded at a constant velocity since the big bang and all galaxies expanded from the ...
... Hubble's Law is the relation between the recession velocity of a galaxy and its distance: Vr = H d, that is, the velocity of recession Vr equals the distance d times the Hubble constant H. Assuming the galaxies have receded at a constant velocity since the big bang and all galaxies expanded from the ...
Lecture 6: Properties of Stars The Constellations The Constellations
... mapped many of these “absorption lines” with reasonable accuracy - called Fraunhofer lines. ‘Na D lines’ ...
... mapped many of these “absorption lines” with reasonable accuracy - called Fraunhofer lines. ‘Na D lines’ ...
8hrdiagram1s
... If you know the luminosity and you measure the flux you can find the distance (F = L/4pd2) Called spectroscopic parallax ...
... If you know the luminosity and you measure the flux you can find the distance (F = L/4pd2) Called spectroscopic parallax ...
Stellar Evolution and the HR Diagram – Study Guide
... c. Which is brighter, the sun or a white dwarf? The Sun (but not as hot) d. Is Vega brighter than our sun? Yes e. Is Antares hotter than our sun? No, it’s a giant, class K or M 22. Stars that move off the main sequence first move to the _Giant_ region of the HR diagram. These stars are fusing __heli ...
... c. Which is brighter, the sun or a white dwarf? The Sun (but not as hot) d. Is Vega brighter than our sun? Yes e. Is Antares hotter than our sun? No, it’s a giant, class K or M 22. Stars that move off the main sequence first move to the _Giant_ region of the HR diagram. These stars are fusing __heli ...
Stellar classification
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Light from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with absorption lines. Each line indicates an ion of a certain chemical element, with the line strength indicating the abundance of that ion. The relative abundance of the different ions varies with the temperature of the photosphere. The spectral class of a star is a short code summarizing the ionization state, giving an objective measure of the photosphere's temperature and density.Most stars are currently classified under the Morgan–Keenan (MK) system using the letters O, B, A, F, G, K, and M, a sequence from the hottest (O type) to the coolest (M type). Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest (e.g. A8, A9, F0, F1 form a sequence from hotter to cooler). The sequence has been expanded with classes for other stars and star-like objects that do not fit in the classical system, such class D for white dwarfs and class C for carbon stars.In the MK system a luminosity class is added to the spectral class using Roman numerals. This is based on the width of certain absorption lines in the star's spectrum which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class 0 or Ia+ stars for hypergiants, class I stars for supergiants, class II for bright giants, class III for regular giants, class IV for sub-giants, class V for main-sequence stars, class sd for sub-dwarfs, and class D for white dwarfs. The full spectral class for the Sun is then G2V, indicating a main-sequence star with a temperature around 5,800K.