Chapter 27 Stars and Galaxies
... Absolute Magnitude Brightness from 32.6 ly Ex: If the sun was 32.6 ly away, it would be a fifth magnitude star. Its absolute magnitude = +5 Most stars are between a -5 and +15 ...
... Absolute Magnitude Brightness from 32.6 ly Ex: If the sun was 32.6 ly away, it would be a fifth magnitude star. Its absolute magnitude = +5 Most stars are between a -5 and +15 ...
Denton ISD
... A galaxy that is moving toward Earth will show — A a red shift in its spectrum B an increase in light-years ...
... A galaxy that is moving toward Earth will show — A a red shift in its spectrum B an increase in light-years ...
the ELECTROMAGNETIC SPECTRUM / WAVE PROPERTIES
... objects, and for sun tanning • Sources: Ultra hot objects 5000°C or more, such as Stars ...
... objects, and for sun tanning • Sources: Ultra hot objects 5000°C or more, such as Stars ...
PowerPoint
... High-mass star forming regions are much more distant (in average) than those of low-mass stars (high-mass: 3-7kpc vs. low-mass: 0.1-0.3 kpc) OB stars - form preferentially in the centre of dense star clusters - seem to live pref. in (tight) binary and higher order systems ...
... High-mass star forming regions are much more distant (in average) than those of low-mass stars (high-mass: 3-7kpc vs. low-mass: 0.1-0.3 kpc) OB stars - form preferentially in the centre of dense star clusters - seem to live pref. in (tight) binary and higher order systems ...
Astronomy 401 Lecture 18 Galaxy Interactions Here we briefly
... enhanced by ram pressure stripping. Ram pressure is the pressure exerted on something moving through a fluid medium, and it creates a strong drag force. As you’d expect, it depends on the velocity at which the object is moving and the density of the medium: ...
... enhanced by ram pressure stripping. Ram pressure is the pressure exerted on something moving through a fluid medium, and it creates a strong drag force. As you’d expect, it depends on the velocity at which the object is moving and the density of the medium: ...
Theoretical Problem 3
... the ratio of mass M to radius R is the same and depends only on physical constants. Find the equation for the ratio M / R for stars fusing hydrogen. ...
... the ratio of mass M to radius R is the same and depends only on physical constants. Find the equation for the ratio M / R for stars fusing hydrogen. ...
AST301.Ch21.StellarExpl - University of Texas Astronomy
... wavelengths (right). The X-rays are emitted because the gas is so hot (~ million degrees K), while the radio emission is from electrons that are gyrating at nearly the speed of light around the strong magnetic field in the remnant—this is where it is believed that cosmic rays are accelerated. ...
... wavelengths (right). The X-rays are emitted because the gas is so hot (~ million degrees K), while the radio emission is from electrons that are gyrating at nearly the speed of light around the strong magnetic field in the remnant—this is where it is believed that cosmic rays are accelerated. ...
Integrative Studies 410 Our Place in the Universe
... Mira Stars • Mira (=wonderful, lat.) [o Ceti]: sometimes visible with bare eye, sometimes faint • Long period variable star: 332 days period • Cool red giants • Sometimes periodic, sometimes irregular • some eject gas into space ...
... Mira Stars • Mira (=wonderful, lat.) [o Ceti]: sometimes visible with bare eye, sometimes faint • Long period variable star: 332 days period • Cool red giants • Sometimes periodic, sometimes irregular • some eject gas into space ...
Spectroscopy – the study of the colors of light (the spectrum) given
... The main sequence can be used to find the distance to a star using the apparent brightness and the temperature (color). This use of a Hertzsprung-Russell diagram to find the distance of very distant stars is called spectroscopic ...
... The main sequence can be used to find the distance to a star using the apparent brightness and the temperature (color). This use of a Hertzsprung-Russell diagram to find the distance of very distant stars is called spectroscopic ...
Space Science Unit
... phase of the star’s life cycle the star is in and other important information about the star. • Most stars are what we consider main sequence (including our sun). They make up 90% of the stars in our sky. These stars are the diagonal strip running through the middle of the chart. ...
... phase of the star’s life cycle the star is in and other important information about the star. • Most stars are what we consider main sequence (including our sun). They make up 90% of the stars in our sky. These stars are the diagonal strip running through the middle of the chart. ...
Level 4 Constellations North Star, South Star
... Constellations are groupings of stars that form easily recognized and remembered patterns, such as Orion and the Big Dipper. The Big Dipper is actually an asterism, not a constellation, because it is only part of the constellation Ursa Major (the Big Bear). Actually, the stars in the majority of all ...
... Constellations are groupings of stars that form easily recognized and remembered patterns, such as Orion and the Big Dipper. The Big Dipper is actually an asterism, not a constellation, because it is only part of the constellation Ursa Major (the Big Bear). Actually, the stars in the majority of all ...
Astronomy Webquest _2 STARS
... several billion years, because they burn their fuel much more slowly. Eventually, however, the ________________ fuel that powers the nuclear reactions within stars will begin to run out, and they will enter the final phases of their lifetime. Over time, they will expand, cool and change color to bec ...
... several billion years, because they burn their fuel much more slowly. Eventually, however, the ________________ fuel that powers the nuclear reactions within stars will begin to run out, and they will enter the final phases of their lifetime. Over time, they will expand, cool and change color to bec ...
A minimum column density of 1gcm(
... galaxies and the dominant energy sources in the Universe today. They form rarely because efficient radiative cooling keeps most star-forming gas clouds close to isothermal as they collapse, and this favours fragmentation into stars of one solar mass or lower1–3. Heating of a cloud by accreting low-m ...
... galaxies and the dominant energy sources in the Universe today. They form rarely because efficient radiative cooling keeps most star-forming gas clouds close to isothermal as they collapse, and this favours fragmentation into stars of one solar mass or lower1–3. Heating of a cloud by accreting low-m ...
te acher`s guide te acher`s guide
... counterparts. Space travelers Adi and Woops help viewers clearly answer each question using computer graphics and space footage. What are the signs of the zodiac? The signs of the zodiac are twelve different groups of stars that are named after animals or mythical creatures.They are constellations — ...
... counterparts. Space travelers Adi and Woops help viewers clearly answer each question using computer graphics and space footage. What are the signs of the zodiac? The signs of the zodiac are twelve different groups of stars that are named after animals or mythical creatures.They are constellations — ...
Slide 1 - Physics @ IUPUI
... the brighter it is (sort of like a bigger bell has a larger period of vibration). • This allows us to measure distances (especially since these are very bright stars which can be seen a LONG distance away)! • In fact, the distance to Andromeda was first attempted to be estimated using Cepheid ...
... the brighter it is (sort of like a bigger bell has a larger period of vibration). • This allows us to measure distances (especially since these are very bright stars which can be seen a LONG distance away)! • In fact, the distance to Andromeda was first attempted to be estimated using Cepheid ...
Microsoft Word
... Most of the stars in the universe form in young clusters and they are the basic units of star formation (Lada \& Lada 2003). Their study can directly address a number of fundamental astrophysical questions such as the origin and early evolution of stars and planetary systems and more importantly the ...
... Most of the stars in the universe form in young clusters and they are the basic units of star formation (Lada \& Lada 2003). Their study can directly address a number of fundamental astrophysical questions such as the origin and early evolution of stars and planetary systems and more importantly the ...
Spectra of stars
... The continuous spectrum originates from the surface of the star and the absorption lines are produced when light passes upwards and outwards through the tenuous upper layers of the star. By looking at the spectrum of a star astronomers can determine: (a) the temperature of the star (b) the velocity ...
... The continuous spectrum originates from the surface of the star and the absorption lines are produced when light passes upwards and outwards through the tenuous upper layers of the star. By looking at the spectrum of a star astronomers can determine: (a) the temperature of the star (b) the velocity ...
Young Galaxies Grow - Astronomical Society of the Pacific
... arms appeared much more extended than seen in visible images of the galaxy. Ultravioletbright, thin structures stretch to almost five times the galaxy’s optical radius. • Another spiral galaxy showed a similar extended Ultraviolet disk. So astronomers began to look at several such galaxies with GAL ...
... arms appeared much more extended than seen in visible images of the galaxy. Ultravioletbright, thin structures stretch to almost five times the galaxy’s optical radius. • Another spiral galaxy showed a similar extended Ultraviolet disk. So astronomers began to look at several such galaxies with GAL ...
May 2017 - What`s Out Tonight?
... cury, Venus, Mars, Jupiter and Saturn. Venus is extremely bright Open clusters reside in our Milky Way Galaxy. Our Sun is no and hugs close to the Sun, so you see it for a short time in the longer in its group. west after sunset or in the east before sunrise. Jupiter can be out Globular Clusters loo ...
... cury, Venus, Mars, Jupiter and Saturn. Venus is extremely bright Open clusters reside in our Milky Way Galaxy. Our Sun is no and hugs close to the Sun, so you see it for a short time in the longer in its group. west after sunset or in the east before sunrise. Jupiter can be out Globular Clusters loo ...
What is a Scientist? - Cockeysville Middle School
... Identify the temperature associated with each color, and include an example of a star that would appear each color. ...
... Identify the temperature associated with each color, and include an example of a star that would appear each color. ...
Stellar Evolution
... carbon core. • How they get from main sequence to the carbon core stage is a little different. • Now however, there is enough mass that it becomes hot enough to fuse carbon? • Hot enough to eventually fuse lots of elements. ...
... carbon core. • How they get from main sequence to the carbon core stage is a little different. • Now however, there is enough mass that it becomes hot enough to fuse carbon? • Hot enough to eventually fuse lots of elements. ...
Practice Questions for Final
... Which of the following does NOT support the theory that active galactic nuclei are powered by accretion disks around massive black holes? A. Spectral lines from the galactic center indicate that clouds of gas are orbiting a central object at very high speed. B. The total amount of radiation coming f ...
... Which of the following does NOT support the theory that active galactic nuclei are powered by accretion disks around massive black holes? A. Spectral lines from the galactic center indicate that clouds of gas are orbiting a central object at very high speed. B. The total amount of radiation coming f ...
Astronomy 10 - UC Berkeley Astronomy w
... M If a star is 3 times as massive then it live 3−2.5 ≈ 0.064 times as long. This should make sense–more luminous stars live a shorter amount of time. (6) page 274, question 35 The cluster that doesn’t have any O, B, A, and F stars (the second one) must be older. The lack of F stars means that the cl ...
... M If a star is 3 times as massive then it live 3−2.5 ≈ 0.064 times as long. This should make sense–more luminous stars live a shorter amount of time. (6) page 274, question 35 The cluster that doesn’t have any O, B, A, and F stars (the second one) must be older. The lack of F stars means that the cl ...
Section 27.2
... stable part of their life cycle. White dwarfs are hot and dim and cannot be seen without a telescope. Red giants are cool and bright and some can be seen without a telescope. Can you locate blue giants on the H-R diagram? ...
... stable part of their life cycle. White dwarfs are hot and dim and cannot be seen without a telescope. Red giants are cool and bright and some can be seen without a telescope. Can you locate blue giants on the H-R diagram? ...
Chapter 19. Mapping the Universe from Herschel to Sloan
... Leavitt of Harvard Observatory who was working on a type of variable star known as Cepheid variables. These objects undergo brightness variations by a factor of two or more that are periodic on time scales of a few days to more than 100 days. The cause of these variations is pulsation of the star. I ...
... Leavitt of Harvard Observatory who was working on a type of variable star known as Cepheid variables. These objects undergo brightness variations by a factor of two or more that are periodic on time scales of a few days to more than 100 days. The cause of these variations is pulsation of the star. I ...
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.