Handout 3 1-2 ppt
... sky. It struck the earth in what is now northern Arizona, exploding with the force of 2 ½ million tons of TNT. ...
... sky. It struck the earth in what is now northern Arizona, exploding with the force of 2 ½ million tons of TNT. ...
powerpoint version
... (the Sun constitutes 99.85% of the total mass of the solar system) Mass divided by volume gives us the Sun’s average density = 1410 kg per cubic metre The Sun is made up of gas - it is too hot to be liquid. PHYS1142 ...
... (the Sun constitutes 99.85% of the total mass of the solar system) Mass divided by volume gives us the Sun’s average density = 1410 kg per cubic metre The Sun is made up of gas - it is too hot to be liquid. PHYS1142 ...
Document
... • If you know how luminous a star REALLY is and how bright it looks from Earth, you can determine how far away it must be to look that faint. • For any star in the sky, we KNOW: ...
... • If you know how luminous a star REALLY is and how bright it looks from Earth, you can determine how far away it must be to look that faint. • For any star in the sky, we KNOW: ...
The Sun Compared to Other Stars
... The Sun Compared to Other Stars • Hertzsprung-Russell (HR) Diagram: A graph plot indicating individual stars as points, with stellar luminosity on the vertical axis & surface temperature (spectral type) on the horizontal axis • We can use spectroscopy to determine the spectral type & luminosity of a ...
... The Sun Compared to Other Stars • Hertzsprung-Russell (HR) Diagram: A graph plot indicating individual stars as points, with stellar luminosity on the vertical axis & surface temperature (spectral type) on the horizontal axis • We can use spectroscopy to determine the spectral type & luminosity of a ...
Stars
... Ball of hot gas (hydrogen and helium) that gives off light Have different colors, sizes, and patterns. ...
... Ball of hot gas (hydrogen and helium) that gives off light Have different colors, sizes, and patterns. ...
Stellar Evolution Diagram Answer Key:
... This is a cloud of dust and gas that can last for millions of years. A nebula consists commonly of about 70% Hydrogen, 28% Helium, and about 2% of other heavier elements. Nebulas rarely start to clump together on their own- often they require an outside force to nudge them into coalescing. Such a fo ...
... This is a cloud of dust and gas that can last for millions of years. A nebula consists commonly of about 70% Hydrogen, 28% Helium, and about 2% of other heavier elements. Nebulas rarely start to clump together on their own- often they require an outside force to nudge them into coalescing. Such a fo ...
Star Formation
... • Interstellar gas, like the sun, is 74% hydrogen and 25% helium. • Interstellar dust, like clouds in the gas giants, are molecular carbon monoxide, ammonia, and water. • Traces of all other elements are present. ...
... • Interstellar gas, like the sun, is 74% hydrogen and 25% helium. • Interstellar dust, like clouds in the gas giants, are molecular carbon monoxide, ammonia, and water. • Traces of all other elements are present. ...
Today`s Powerpoint
... If a star is moving rapidly towards Earth then its spectrum will be: A: the same as if it were at rest B: shifted to the blue C: shifted to the red D: much brighter than if it were at rest E: much fainter than if it were at rest ...
... If a star is moving rapidly towards Earth then its spectrum will be: A: the same as if it were at rest B: shifted to the blue C: shifted to the red D: much brighter than if it were at rest E: much fainter than if it were at rest ...
StarType
... à=Ð/Ð8Types of Stars When you look at the stars you’ll notice that some are white, some are yellow, and some are red. Stars are classified according to their colors, ranging from electric blue for the hottest stars to dull red for the coolest stars. Early spectrometers identified emission lines in t ...
... à=Ð/Ð8Types of Stars When you look at the stars you’ll notice that some are white, some are yellow, and some are red. Stars are classified according to their colors, ranging from electric blue for the hottest stars to dull red for the coolest stars. Early spectrometers identified emission lines in t ...
Stars from Afar
... An HR diagram shows the two most important characteristics of stars, which are temperature and absolute magnitude (brightness) and/or luminosity. ...
... An HR diagram shows the two most important characteristics of stars, which are temperature and absolute magnitude (brightness) and/or luminosity. ...
Stars - Independence High School
... • Seasonal- Orbit equator and can only be seen during certain times of the year ...
... • Seasonal- Orbit equator and can only be seen during certain times of the year ...
Lecture Summary (11/22)
... billion years. More massive stars have shorter main sequence lifetimes; lower mass stars have longer main sequence lifetimes. Stars more massive than the Sun are born as protostars in nebulae. Due to their great mass, they are forced to fuse hydrogen into helium at a higher core temperature and cons ...
... billion years. More massive stars have shorter main sequence lifetimes; lower mass stars have longer main sequence lifetimes. Stars more massive than the Sun are born as protostars in nebulae. Due to their great mass, they are forced to fuse hydrogen into helium at a higher core temperature and cons ...
the evolutionary radial distributions of h2 density within spiral and
... may be detected with ALMA, we need to transform the limiting flux for this instrument to a limit in gas density. The flux limit depends on the observed frecuency. We take the highest value from the report “Science with ALMA”, and we use Eq. 1 from Solomon and Vanden Bout (2005), to calculate the min ...
... may be detected with ALMA, we need to transform the limiting flux for this instrument to a limit in gas density. The flux limit depends on the observed frecuency. We take the highest value from the report “Science with ALMA”, and we use Eq. 1 from Solomon and Vanden Bout (2005), to calculate the min ...
Lecture 12: Age, Metalicity, and Observations Abundance
... SFR(M " yr #1 ) = 7.9 $10#42 L(H% )(ergs#1 ) = 1.08 $10#53 Q(H o )(s#1 ) Q(H o ) is the ionising photon luminosity constants are derived from evol. synthesis models (e.g., Kennicutt 1982) ...
... SFR(M " yr #1 ) = 7.9 $10#42 L(H% )(ergs#1 ) = 1.08 $10#53 Q(H o )(s#1 ) Q(H o ) is the ionising photon luminosity constants are derived from evol. synthesis models (e.g., Kennicutt 1982) ...
Astronomy 1 Study Guide Key 16
... 1. Rank to following words in order of their size – largest to smallest: universe, planet, moon, solar system, galaxy, super giant, red giant, main sequence star. Moon – planet – main sequence star – red giant – supergiant – solar system – galaxy – universe 2. How do we measure distance in space? li ...
... 1. Rank to following words in order of their size – largest to smallest: universe, planet, moon, solar system, galaxy, super giant, red giant, main sequence star. Moon – planet – main sequence star – red giant – supergiant – solar system – galaxy – universe 2. How do we measure distance in space? li ...
Learning Targets
... 15.2 Characteristics of Stars 1. I am able to state the characteristics used for classifying stars. 2. I know how to describe what a light-year is. 3. I know how to use a Hertzsprung-Russell diagram to classify stars. 15.3 Lives of Stars 4. I am able to state the life cycle of small and large stars. ...
... 15.2 Characteristics of Stars 1. I am able to state the characteristics used for classifying stars. 2. I know how to describe what a light-year is. 3. I know how to use a Hertzsprung-Russell diagram to classify stars. 15.3 Lives of Stars 4. I am able to state the life cycle of small and large stars. ...
The Life Cycle of Stars Webquest
... Continue to read on to the section “A Nuclear Furnace” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. The nuclear reactions inside a star, such as our sun, convert hydrogen into helium by means of a process known as. 2. What gives a star its ener ...
... Continue to read on to the section “A Nuclear Furnace” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. The nuclear reactions inside a star, such as our sun, convert hydrogen into helium by means of a process known as. 2. What gives a star its ener ...
Astronomy and Our Origins
... • Doppler Effect Things moving away shift to Redder colors = longer distances & longer wavelengths = red shift Things moving towards us shift to Bluer colors = shorter distances & shorter wavelengths = blue shift ...
... • Doppler Effect Things moving away shift to Redder colors = longer distances & longer wavelengths = red shift Things moving towards us shift to Bluer colors = shorter distances & shorter wavelengths = blue shift ...
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... Semimajor axis Kepler’s second law of motion Kepler’s third law of motion Newton to the rescue ...
... Semimajor axis Kepler’s second law of motion Kepler’s third law of motion Newton to the rescue ...
the life cycle of stars - North American Montessori Center
... sun, like all yellow dwarf stars, entered the main sequence, the main portion of the life cycle of an average star, in which it converts hydrogen into helium steadily for billions of years. It takes an average star like the sun 10 billion years to convert the hydrogen in its core to helium. The sun ...
... sun, like all yellow dwarf stars, entered the main sequence, the main portion of the life cycle of an average star, in which it converts hydrogen into helium steadily for billions of years. It takes an average star like the sun 10 billion years to convert the hydrogen in its core to helium. The sun ...
Star Classification
... Star Classification The first people to combine a camera with a spectroscope were the father and son team of John and Henry Draper in the 1870s. Their work was carried on by Edward C. Pickering who, by 1918, had listed the spectra of over 200000 stars. Using details about luminosity and composition, ...
... Star Classification The first people to combine a camera with a spectroscope were the father and son team of John and Henry Draper in the 1870s. Their work was carried on by Edward C. Pickering who, by 1918, had listed the spectra of over 200000 stars. Using details about luminosity and composition, ...
©M. Rieke 1 Correct responses in BOLDFACE. 1. Why did
... a. at the end the electrons in the atoms have gone to lower energy levels and given off the energy they lost b. the atoms join together into bigger molecules, and the molecular binding energy is released c. the fusion products weigh a little less than the input materials, and the mass that is lost a ...
... a. at the end the electrons in the atoms have gone to lower energy levels and given off the energy they lost b. the atoms join together into bigger molecules, and the molecular binding energy is released c. the fusion products weigh a little less than the input materials, and the mass that is lost a ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.