Slide 1
... 1. Stars starting with less than about 2 Msun finish burning to carbon, become unstable as they burn H and He in a shell and shuck off a shell of 10-20% of their mass, becoming a planetary nebula, glowing because they are ionized by the hot UV core. ...
... 1. Stars starting with less than about 2 Msun finish burning to carbon, become unstable as they burn H and He in a shell and shuck off a shell of 10-20% of their mass, becoming a planetary nebula, glowing because they are ionized by the hot UV core. ...
Properties of Stars: The H
... • But a plot of Luminosity vs color (or spectral type or temperature) is called a Hertzsprung-Russell Diagram and shows some interesting sequences. Red Giants ...
... • But a plot of Luminosity vs color (or spectral type or temperature) is called a Hertzsprung-Russell Diagram and shows some interesting sequences. Red Giants ...
Chapter19
... greater speed and hear a click as the two cars bang into one another (before being pushed apart). I finish by asking what would happen if the magnets were stronger, simulating nuclei of greater charge. This sounds pretty simple-minded, but I find it helps students who have no feeling for electric ch ...
... greater speed and hear a click as the two cars bang into one another (before being pushed apart). I finish by asking what would happen if the magnets were stronger, simulating nuclei of greater charge. This sounds pretty simple-minded, but I find it helps students who have no feeling for electric ch ...
Star Evolution
... fusion in their cores. They leave the main sequence and become red giants when the core hydrogen is depleted” ...
... fusion in their cores. They leave the main sequence and become red giants when the core hydrogen is depleted” ...
Earth Science Notes
... Hetzsprung and Russell developed a graph that shows the relationship between luminosity and temperature. ...
... Hetzsprung and Russell developed a graph that shows the relationship between luminosity and temperature. ...
Nuclear fusion in stars
... gravity acts to collapse it, while thermal motions due to heat try to take it apart Large molecular clouds are generally stable, but they can be broken into smaller, denser, and unstable fragments. Instability is triggered by shock waves Such waves may be caused by supernova explosions, birth events ...
... gravity acts to collapse it, while thermal motions due to heat try to take it apart Large molecular clouds are generally stable, but they can be broken into smaller, denser, and unstable fragments. Instability is triggered by shock waves Such waves may be caused by supernova explosions, birth events ...
The Hidden Lives of Galaxies NSTA 2001
... Do small stars or large stars burn faster? Do small stars or large stars burn hotter? When does fusion stop in a red supergiant? Why? What determines the life cycle of a star? Where do stars begin to form? Why are type IA supernovae rare? How would you list the stars in color from hott ...
... Do small stars or large stars burn faster? Do small stars or large stars burn hotter? When does fusion stop in a red supergiant? Why? What determines the life cycle of a star? Where do stars begin to form? Why are type IA supernovae rare? How would you list the stars in color from hott ...
Aging nearby spiral galaxies using H
... » Combine theories of physical stellar proerties: mass loss, spectral output, plasma/gas dynamics &c. » Different options to cover most types of conditions: ...
... » Combine theories of physical stellar proerties: mass loss, spectral output, plasma/gas dynamics &c. » Different options to cover most types of conditions: ...
30-2 Directed Reading
... b. stays on the main sequence for about 10 billion years. c. stays on the main sequence for about 14 billion years. d. stays on the main sequence for about 100 billion years. LEAVING THE MAIN SEQUENCE ...
... b. stays on the main sequence for about 10 billion years. c. stays on the main sequence for about 14 billion years. d. stays on the main sequence for about 100 billion years. LEAVING THE MAIN SEQUENCE ...
Earth Science, 10th edition Chapter 23: Beyond Our Solar System I
... 1. Dim stars have large numbers a. First magnitude appear brighter b. Sixth magnitude are the faintest stars visible to the eye 2. Negative numbers are also used 2. Absolute magnitude a. "True" or intrinsic brightness of a star b. Brightness at a standard distance of 32.6 light-years c. Most stars' ...
... 1. Dim stars have large numbers a. First magnitude appear brighter b. Sixth magnitude are the faintest stars visible to the eye 2. Negative numbers are also used 2. Absolute magnitude a. "True" or intrinsic brightness of a star b. Brightness at a standard distance of 32.6 light-years c. Most stars' ...
Deep Space Objects
... clusters), new subdivisions (younger open star clusters) and rough parts of town (black holes). Here’s a closer look at some of the neighbourhoods you might run into on a faster-than-light trip through our home in deep space: Stars Like the different colours of a flame, hotter stars burn yellow, whi ...
... clusters), new subdivisions (younger open star clusters) and rough parts of town (black holes). Here’s a closer look at some of the neighbourhoods you might run into on a faster-than-light trip through our home in deep space: Stars Like the different colours of a flame, hotter stars burn yellow, whi ...
White Dwarfs and Neutron Stars
... and create an X-ray burster • Can collide or merge with each other (or black holes), creating a gamma ray burst (the most powerful explosions in the ...
... and create an X-ray burster • Can collide or merge with each other (or black holes), creating a gamma ray burst (the most powerful explosions in the ...
The Big Dipper Constellation
... The Big Dipper What is a Constellation? From very early times, man has been fascinated by the stars. Early stargazers began naming stars. They also noticed patterns of stars that appeared night after night in the sky. These patterns or groupings of stars are called constellations. They also began to ...
... The Big Dipper What is a Constellation? From very early times, man has been fascinated by the stars. Early stargazers began naming stars. They also noticed patterns of stars that appeared night after night in the sky. These patterns or groupings of stars are called constellations. They also began to ...
Question C:
... The easy way is to look up B−V=−0.30 for a B0V star in table A4-3, so B=2.5−0.3=2.2. The hard way is to first get the temperature of a B0 star from Figure 13-6 (25,000K), and calculate B−V=−0.52 using Equation 11-11a (although it is not meant for such hot stars). c. (5 pt): In a certain star, hydrog ...
... The easy way is to look up B−V=−0.30 for a B0V star in table A4-3, so B=2.5−0.3=2.2. The hard way is to first get the temperature of a B0 star from Figure 13-6 (25,000K), and calculate B−V=−0.52 using Equation 11-11a (although it is not meant for such hot stars). c. (5 pt): In a certain star, hydrog ...
Stars
... Hetzsprung and Russell developed a graph that shows the relationship between luminosity and temperature. ...
... Hetzsprung and Russell developed a graph that shows the relationship between luminosity and temperature. ...
Slide 1
... shell produce more energy than needed for pressure support Expansion and cooling of the outer layers of the star Red ...
... shell produce more energy than needed for pressure support Expansion and cooling of the outer layers of the star Red ...
Triggered Star Formation by Massive Stars in Star
... A triggered star formation process has several imprints which can be observationally diagnosed: • The remnant cloud is extended toward, or pointing to, the massive stars. • The young stellar groupings in the region are roughly lined up between the remnant cloud and the luminous star. • Stars closer ...
... A triggered star formation process has several imprints which can be observationally diagnosed: • The remnant cloud is extended toward, or pointing to, the massive stars. • The young stellar groupings in the region are roughly lined up between the remnant cloud and the luminous star. • Stars closer ...
Assignment 3 - Physics Internal Website
... The stellar temperature axis is often characterized by spectral classification rather than temperature. The standard spectral classification goes as O, B, A, F, G, K, M, (and for brown dwarfs L, T). The earlier in the alphabet the more prominent the H Balmer series, so A stars have the most promine ...
... The stellar temperature axis is often characterized by spectral classification rather than temperature. The standard spectral classification goes as O, B, A, F, G, K, M, (and for brown dwarfs L, T). The earlier in the alphabet the more prominent the H Balmer series, so A stars have the most promine ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... different masses but with the same age . Lets make a plot of Log(L/L) vs. LogTeff for an age of 1Gyr. The result is an isochrone. Important - think about what we are looking at when we observe a cluster. We are seeing a “freeze-frame” picture at a particular age. We see how stars of different masse ...
... different masses but with the same age . Lets make a plot of Log(L/L) vs. LogTeff for an age of 1Gyr. The result is an isochrone. Important - think about what we are looking at when we observe a cluster. We are seeing a “freeze-frame” picture at a particular age. We see how stars of different masse ...
Quantum Well Electron Gain Structures and Infrared
... Jupiter, Saturn, Uranus, Neptune too cold (though some moons may be OK) ...
... Jupiter, Saturn, Uranus, Neptune too cold (though some moons may be OK) ...
CHARACTERISTICS OF STARS
... looks from Earth depends on both its distance and how bright the star actually is. The brightness of a star can be described in 2 different ways: apparent brightness and absolute brightness. A star’s apparent brightness is its brightness as seen from Earth. Astronomers can measure apparent brightnes ...
... looks from Earth depends on both its distance and how bright the star actually is. The brightness of a star can be described in 2 different ways: apparent brightness and absolute brightness. A star’s apparent brightness is its brightness as seen from Earth. Astronomers can measure apparent brightnes ...
Chapter 15 Surveying the Stars
... • What are giants, supergiants, and white dwarfs? – All stars become larger and redder after core hydrogen burning is exhausted: giants and supergiants – Most stars end up as tiny white dwarfs after ...
... • What are giants, supergiants, and white dwarfs? – All stars become larger and redder after core hydrogen burning is exhausted: giants and supergiants – Most stars end up as tiny white dwarfs after ...
read in advance to speed your work
... seen when we look in the direction of the constellation of Orion. Begin making an H-R diagram for the stars in Orion (Table II). Plot the MV values (MV again is simply absolute magnitude, M, with the subscript indicating that the magnitude is measured in the visual part of the spectrum) against the ...
... seen when we look in the direction of the constellation of Orion. Begin making an H-R diagram for the stars in Orion (Table II). Plot the MV values (MV again is simply absolute magnitude, M, with the subscript indicating that the magnitude is measured in the visual part of the spectrum) against the ...
PREVIEW-Reading Quiz 06 - Chapter 12
... from this quantum mechanical effect, it is insensitive to temperature, i.e., the pressure doesn't go down as the star cools. This pressure is known as electron degeneracy pressure and it is the force that supports white dwarf stars against their own gravity." This means only 2 electrons in the lowes ...
... from this quantum mechanical effect, it is insensitive to temperature, i.e., the pressure doesn't go down as the star cools. This pressure is known as electron degeneracy pressure and it is the force that supports white dwarf stars against their own gravity." This means only 2 electrons in the lowes ...
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.