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... an eruption that cause the WD to temporarily “flair up” (10 magnitudes higher or more), this is called a nova and the process can be reoccurring. The most massive stars can get hot enough to fuse carbon and other elements. After they go through the giant stage they eventually fuse elements through ...
... an eruption that cause the WD to temporarily “flair up” (10 magnitudes higher or more), this is called a nova and the process can be reoccurring. The most massive stars can get hot enough to fuse carbon and other elements. After they go through the giant stage they eventually fuse elements through ...
File
... A _____________, on the other hand, is a large amount of gas and dust spread out in an immense volume. All stars begin their lives as parts of nebulas. ______________ can pull some of the gas and dust in a nebula together. The contracting cloud is then called a _________________________. P ...
... A _____________, on the other hand, is a large amount of gas and dust spread out in an immense volume. All stars begin their lives as parts of nebulas. ______________ can pull some of the gas and dust in a nebula together. The contracting cloud is then called a _________________________. P ...
Astronomy Unit Outline
... Describe the different models of the universe and the evidence that supports each model. Describe the structure of the Milky Way Describe and identify different types of galaxies Describe the difference between the two spectra Describe the information that can be found in the spectra. ...
... Describe the different models of the universe and the evidence that supports each model. Describe the structure of the Milky Way Describe and identify different types of galaxies Describe the difference between the two spectra Describe the information that can be found in the spectra. ...
Basic Properties of Stars
... sense. According to the blackbody law, hot things emit more light. But a star’s brightness also depends on its size – the larger the area, the more square centimeters are emitting and the more light you get. The relationship between luminosity, radius, and temperature is ...
... sense. According to the blackbody law, hot things emit more light. But a star’s brightness also depends on its size – the larger the area, the more square centimeters are emitting and the more light you get. The relationship between luminosity, radius, and temperature is ...
Surveys of Stars, The interstellar medium
... If a star is half as hot as our Sun, but has the same luminosity, how large is its radius compared to the Sun? 1) ½ times as large 2) ¼ times as large 3) 4 times larger 4) the same ...
... If a star is half as hot as our Sun, but has the same luminosity, how large is its radius compared to the Sun? 1) ½ times as large 2) ¼ times as large 3) 4 times larger 4) the same ...
Slide 1
... • L does not increase at the onset of the He-flash itself since the central region of the core is quite opaque • The H-burning shell is slowly extinguished and L decreases, even as the star shrinks and temperature rises; the star moves leftward along a nearly Horizontal Branch on the H-R diagram • L ...
... • L does not increase at the onset of the He-flash itself since the central region of the core is quite opaque • The H-burning shell is slowly extinguished and L decreases, even as the star shrinks and temperature rises; the star moves leftward along a nearly Horizontal Branch on the H-R diagram • L ...
30-1
... 6. What is the most common element in stars? What is the second most common element? _______________________________________________________________ ...
... 6. What is the most common element in stars? What is the second most common element? _______________________________________________________________ ...
L7 - QUB Astrophysics Research Centre
... The observed mass-luminosity law is not a simple power law but if the central part of the curve (corresponding to close to a solar mass) is approximated by a power law, it has an exponent of approximately 5. Which is in good agreement with the value of 5.46 above. Similarly the lower part of the mai ...
... The observed mass-luminosity law is not a simple power law but if the central part of the curve (corresponding to close to a solar mass) is approximated by a power law, it has an exponent of approximately 5. Which is in good agreement with the value of 5.46 above. Similarly the lower part of the mai ...
Introduction:
... slow rotator. This would mean that the pulsation periods of the star would be much smaller than its rotation period. To validate this assumption, they used mathematical theories to compute estimates of pulsation periods for a given rotation speed. They then compared their calculated values to those ...
... slow rotator. This would mean that the pulsation periods of the star would be much smaller than its rotation period. To validate this assumption, they used mathematical theories to compute estimates of pulsation periods for a given rotation speed. They then compared their calculated values to those ...
Observational properties of stars
... many stars at once, particularly those with a common origin. Typically one would look at the characteristics of a cluster of stars. The observable characteristics (surface temperature and luminosity) of stars in clusters have a very specific arrangements on the H-R diagram based upon several charact ...
... many stars at once, particularly those with a common origin. Typically one would look at the characteristics of a cluster of stars. The observable characteristics (surface temperature and luminosity) of stars in clusters have a very specific arrangements on the H-R diagram based upon several charact ...
Lecture 21
... • This inward motion tends to compress the layer, which heats up and becomes more opaque to radiation. • Since radiation diffuses more slowly through the layer (as a consequence of its increased opacity), heat builds up beneath it. N.B. N.B. These These diagrams diagrams are are definitely definitel ...
... • This inward motion tends to compress the layer, which heats up and becomes more opaque to radiation. • Since radiation diffuses more slowly through the layer (as a consequence of its increased opacity), heat builds up beneath it. N.B. N.B. These These diagrams diagrams are are definitely definitel ...
Exercises - Leiden Observatory
... (b) Verify eq. (4.25), and show that the corresponding constant K depends on molecular weight ...
... (b) Verify eq. (4.25), and show that the corresponding constant K depends on molecular weight ...
Chapter 12. Basic Equations of Stellar Structure
... To understand the H-R diagram we must first understand the basic structure of a star and then how they evolve. Prior to 1905, it was not understood how a star could power itself. That is, the luminosity of the Sun is so large that it could not last for more than about 20 million years on the basis o ...
... To understand the H-R diagram we must first understand the basic structure of a star and then how they evolve. Prior to 1905, it was not understood how a star could power itself. That is, the luminosity of the Sun is so large that it could not last for more than about 20 million years on the basis o ...
Lesson 4. Wiens and Stefans Laws
... 1. The peak intensity of thermal radiation from the Sun is at a wavelength of 500 nm, calculate the surface temperature of the Sun. 2. A star has a power output of 6.0 x 1028 W and a surface temperature of 3400K, calculate its radius and the ratio to the Sun’s radius (rsun = 7 x 108 m) ...
... 1. The peak intensity of thermal radiation from the Sun is at a wavelength of 500 nm, calculate the surface temperature of the Sun. 2. A star has a power output of 6.0 x 1028 W and a surface temperature of 3400K, calculate its radius and the ratio to the Sun’s radius (rsun = 7 x 108 m) ...
Life Cycle of a Star - Intervention Worksheet
... become later in its life; typically have the same ...
... become later in its life; typically have the same ...
Lecture 11: The Internal Structure of Stars
... Central Pressure and Temperature in the Sun The observation that the Sun is in hydrostatic equilibrium (along with the mass and radius) gives us enough information to estimate the central pressure and temperature of the Sun. We can use the mass and the radius to estimate how much the force of gravit ...
... Central Pressure and Temperature in the Sun The observation that the Sun is in hydrostatic equilibrium (along with the mass and radius) gives us enough information to estimate the central pressure and temperature of the Sun. We can use the mass and the radius to estimate how much the force of gravit ...
The Life Cycles of Stars
... A star’s life cycle is determined by its mass. The larger the mass, the shorter the life cycle. A star’s mass is determined by the amount of matter that is available in its nebula, the giant cloud of gas and dust in which it is born. Over time, gravity pulls the hydrogen gas in the nebula together a ...
... A star’s life cycle is determined by its mass. The larger the mass, the shorter the life cycle. A star’s mass is determined by the amount of matter that is available in its nebula, the giant cloud of gas and dust in which it is born. Over time, gravity pulls the hydrogen gas in the nebula together a ...
Document
... The Main Sequence Phase – low mass stars Very small stars (< 0.3 solar masses) are fully convective Small and intermediate mass stars have radiative cores and convective envelopes – the higher the mass of the star, the smaller the convective zone The location of the convective layer may change as t ...
... The Main Sequence Phase – low mass stars Very small stars (< 0.3 solar masses) are fully convective Small and intermediate mass stars have radiative cores and convective envelopes – the higher the mass of the star, the smaller the convective zone The location of the convective layer may change as t ...
Ay 112 Midterm review
... light, T4 erg/(cm2 s). The wavelength where the emission is a maximum is given by Wiens law, 0.289 Angstroms/Teff. The luminosity of the star is given by its area ...
... light, T4 erg/(cm2 s). The wavelength where the emission is a maximum is given by Wiens law, 0.289 Angstroms/Teff. The luminosity of the star is given by its area ...
Exercise 4 (Stars and the universe) Suggested answers
... fingerprints” of the elements and are unique for each element, thus the chemical composition of the atmosphere of the star can be obtained. 2. (a) Luminosity L of a celestial body is the actual amount of electromagnetic radiation emitted by the body in each second. (b) ...
... fingerprints” of the elements and are unique for each element, thus the chemical composition of the atmosphere of the star can be obtained. 2. (a) Luminosity L of a celestial body is the actual amount of electromagnetic radiation emitted by the body in each second. (b) ...
the spectrum of a partially ionized jet sodium ionization in t
... We present the results of a study of the sodium ionization and excitation in the winds of low-luminosity, pre-main-sequence stars. Line profiles for the Nal doublet at 5990,5986 Aare discussed and compared with the observations for those T Tauri stars with P-Cygni profiles. We find that the observed ...
... We present the results of a study of the sodium ionization and excitation in the winds of low-luminosity, pre-main-sequence stars. Line profiles for the Nal doublet at 5990,5986 Aare discussed and compared with the observations for those T Tauri stars with P-Cygni profiles. We find that the observed ...
powerpoint file - QUB Astrophysics Research Centre
... The observed mass-luminosity law is not a simple power law but if the central part of the curve (corresponding to close to a solar mass) is approximated by a power law, it has an exponent of approximately 5. Which is in good agreement with the value of 5.46 above. Similarly the lower part of the mai ...
... The observed mass-luminosity law is not a simple power law but if the central part of the curve (corresponding to close to a solar mass) is approximated by a power law, it has an exponent of approximately 5. Which is in good agreement with the value of 5.46 above. Similarly the lower part of the mai ...
HR Diagram, Star Clusters, and Stellar Evolution
... cannot begin to fuse until the temperature of the core reaches 100 million K. How a star begins He fusion depends on its mass: • M > 3 M stars contract rapidly, their cores heat up, and He fusion begins gradually • Less massive stars evolve more slowly and their cores contract so much that degene ...
... cannot begin to fuse until the temperature of the core reaches 100 million K. How a star begins He fusion depends on its mass: • M > 3 M stars contract rapidly, their cores heat up, and He fusion begins gradually • Less massive stars evolve more slowly and their cores contract so much that degene ...
Read the information on Hertzsprung
... In the Hertzsprung-Russell (HR) diagram, each star is represented by a dot. There are lots of stars out there, so there are lots of dots. The position of each dot on the diagram tells us two things about each star: its luminosity and its temperature. The vertical axis represents the star’s luminosit ...
... In the Hertzsprung-Russell (HR) diagram, each star is represented by a dot. There are lots of stars out there, so there are lots of dots. The position of each dot on the diagram tells us two things about each star: its luminosity and its temperature. The vertical axis represents the star’s luminosit ...