Pulsating variable stars and the Hertzsprung
... stars in different stages of their evolution. It is a plot showing a relationship between luminosity (or absolute magnitude) and stars' surface temperature (or spectral type). The bottom scale is ranging from high-temperature blue-white stars (left side of the diagram) to low-temperature red stars ( ...
... stars in different stages of their evolution. It is a plot showing a relationship between luminosity (or absolute magnitude) and stars' surface temperature (or spectral type). The bottom scale is ranging from high-temperature blue-white stars (left side of the diagram) to low-temperature red stars ( ...
The Evolution of Stars - a More Detailed Picture (Chapter 8
... As the star expands, however, the effective temperature cannot continue to fall indefinitely. When the temperature of the outer layers of the star fall below a certain level, they become fully convective. This enables a greater luminosity to be carried by the outer layers and hence abruptly forces ...
... As the star expands, however, the effective temperature cannot continue to fall indefinitely. When the temperature of the outer layers of the star fall below a certain level, they become fully convective. This enables a greater luminosity to be carried by the outer layers and hence abruptly forces ...
Name: Astronomy Lab: The Hertzsprung-Russell (H
... Sometimes the student of astronomy starts to become overwhelmed trying to understand the many measurements and observations astronomers make. Data concerning distance, brightness, color, spectral class, mass, temperature, motion, etc. all seem to be gathered in an attempt to impress the student with ...
... Sometimes the student of astronomy starts to become overwhelmed trying to understand the many measurements and observations astronomers make. Data concerning distance, brightness, color, spectral class, mass, temperature, motion, etc. all seem to be gathered in an attempt to impress the student with ...
10 Stellar Evolution - Journigan-wiki
... Do more stars form in isolation or in groups? Why? What is infall? Why is infall important to protostars? When kinetic energy is transferred to a supercompacted gas, it turns into what? 5. You see a planetary nebula through a telescope. What do you know about it and its history? 6. You see a red gia ...
... Do more stars form in isolation or in groups? Why? What is infall? Why is infall important to protostars? When kinetic energy is transferred to a supercompacted gas, it turns into what? 5. You see a planetary nebula through a telescope. What do you know about it and its history? 6. You see a red gia ...
Powerpoint - BU Imaging Science
... – Astrometry. Watch position of star in sky – Doppler shift. Detect motion of star as both star and planet orbit their centre of mass – Transit. Star’s brightness drops when it is obscured by planet ...
... – Astrometry. Watch position of star in sky – Doppler shift. Detect motion of star as both star and planet orbit their centre of mass – Transit. Star’s brightness drops when it is obscured by planet ...
Supernovae and supernova remnants
... Z is the atomic number) existed. This energy gap hindered the creation of elements beyond helium in the first 3-minute after the Big Bang. In contrast, the universe today is abundant in high-Z elements. In the first epoch of the universe, matter was partly clustered and formed into stars. Once the s ...
... Z is the atomic number) existed. This energy gap hindered the creation of elements beyond helium in the first 3-minute after the Big Bang. In contrast, the universe today is abundant in high-Z elements. In the first epoch of the universe, matter was partly clustered and formed into stars. Once the s ...
Visual Measurements of the Multiple Star
... tronomic eyepiece is being used without a Barlow lens 8.1 with a position angle of 210 degrees and a separaand cannot effectively measure dim stars or ones with tion of 0.3 arc seconds (Mason 2009). This separation small separations. The choice of neglected double was just within the Dawes limit for ...
... tronomic eyepiece is being used without a Barlow lens 8.1 with a position angle of 210 degrees and a separaand cannot effectively measure dim stars or ones with tion of 0.3 arc seconds (Mason 2009). This separation small separations. The choice of neglected double was just within the Dawes limit for ...
The galactic metallicity gradient Martín Hernández, Nieves Leticia
... period of life of the star also depends sensitively on the mass. Hence, the more massive a star is, the more rapidly it exhausts its hydrogen supply. For instance , the expected lifetime of a star ten times more massive than the Sun is about ten million (10 000 000) years, compared to the ten thousa ...
... period of life of the star also depends sensitively on the mass. Hence, the more massive a star is, the more rapidly it exhausts its hydrogen supply. For instance , the expected lifetime of a star ten times more massive than the Sun is about ten million (10 000 000) years, compared to the ten thousa ...
The Milky Way Galaxy
... the Galaxy, where extinction effects are much less than that found along the Milky Way ...
... the Galaxy, where extinction effects are much less than that found along the Milky Way ...
Lecture21
... the surface at a velocity 0.6% the speed of light. • Must use general relativity to model correctly ...
... the surface at a velocity 0.6% the speed of light. • Must use general relativity to model correctly ...
a to z of astronomy
... DARK CLOUD A relatively dense cloud of interstellar material containing dust particles. The dust particles absorb light from the more distant stars etc, so that the region appears dark compared with its surroundings. The clouds are often of low temperature and contain many molecules. DARK MATTER Mat ...
... DARK CLOUD A relatively dense cloud of interstellar material containing dust particles. The dust particles absorb light from the more distant stars etc, so that the region appears dark compared with its surroundings. The clouds are often of low temperature and contain many molecules. DARK MATTER Mat ...
Measuring Radii and Temperatures of Stars
... determined milli-arcsec parallaxes for more than 100,000 stars. • Distances are no longer the major source of uncertainty in radius determinations for many stars • Zillions of stars within range of the Keck interferometer (3 mas at 2m) ...
... determined milli-arcsec parallaxes for more than 100,000 stars. • Distances are no longer the major source of uncertainty in radius determinations for many stars • Zillions of stars within range of the Keck interferometer (3 mas at 2m) ...
Patterns in the Night Sky
... Although we can mark out the same constellations our ancient ancestors saw thousands of years ago, their component stars are not in exactly the same location as they were then. Precise observations of stars reveal that they move relative to each other in space, but these changes in position occur s ...
... Although we can mark out the same constellations our ancient ancestors saw thousands of years ago, their component stars are not in exactly the same location as they were then. Precise observations of stars reveal that they move relative to each other in space, but these changes in position occur s ...
Cepheid
... their general characteristics and behaviour. Most interestingly, exactly how bright is a typical Cepheid star? That requires determining its distance. But the rarity of Cepheids means that even the closest ones are too far away for parallax measurements, and they are often often seen behind lots of ...
... their general characteristics and behaviour. Most interestingly, exactly how bright is a typical Cepheid star? That requires determining its distance. But the rarity of Cepheids means that even the closest ones are too far away for parallax measurements, and they are often often seen behind lots of ...
No Slide Title
... very stable pulsation modes. The presence of a planet will be revealed in anomalous timings, just as with pulsar planets ...
... very stable pulsation modes. The presence of a planet will be revealed in anomalous timings, just as with pulsar planets ...
AST1100 Lecture Notes
... to about 10R⊙ . Giant stars fall in the range between 10R⊙ to about 100R⊙ whereas super giants may have radii of several 100 solar radii. The masses of stars range from 0.08M⊙ for the least massive stars up to about 100M⊙ for the most massive stars. We will later discuss theoretical arguments expla ...
... to about 10R⊙ . Giant stars fall in the range between 10R⊙ to about 100R⊙ whereas super giants may have radii of several 100 solar radii. The masses of stars range from 0.08M⊙ for the least massive stars up to about 100M⊙ for the most massive stars. We will later discuss theoretical arguments expla ...
FROM MOLECULAR CLOUDS TO STARS 1 Star formation and the
... Fig. 7 shows the distribution of line widths observed in dense cores with and without sources detected by the Infrared Astronomical Satellite (IRAS). Cores with new formed stars, detected as infrared sources, have larger line widths (that can not be explained by temperature changes, nearly equal in ...
... Fig. 7 shows the distribution of line widths observed in dense cores with and without sources detected by the Infrared Astronomical Satellite (IRAS). Cores with new formed stars, detected as infrared sources, have larger line widths (that can not be explained by temperature changes, nearly equal in ...
Chapter 17 Star Stuff
... • Changes in brightness or temperature show up on the H-R Diagram • Dying stars form their own branch away from the main sequence line ...
... • Changes in brightness or temperature show up on the H-R Diagram • Dying stars form their own branch away from the main sequence line ...
Chapter 14 Stellar Corpses Stellar Corpses White Dwarfs White
... • Massive stars greater than 10 M upon collapse compress their cores so much that no pressure is capable of supporting it – a black hole results • A black hole is an “object” (region of space) that has an escape velocity that exceeds the speed of light – hence the name – Using the equation for the ...
... • Massive stars greater than 10 M upon collapse compress their cores so much that no pressure is capable of supporting it – a black hole results • A black hole is an “object” (region of space) that has an escape velocity that exceeds the speed of light – hence the name – Using the equation for the ...
chapter18StarDeath
... — Use orbital properties of companion — Measure velocity and distance of orbiting gas It’s a black hole if it’s not a star and its mass exceeds the neutron star limit (~3 MSun) ...
... — Use orbital properties of companion — Measure velocity and distance of orbiting gas It’s a black hole if it’s not a star and its mass exceeds the neutron star limit (~3 MSun) ...
Chapter 18 The Bizarre Stellar Graveyard What is a white dwarf
... – A black hole is a massive object whose radius is so small that the escape velocity exceeds the speed of light ...
... – A black hole is a massive object whose radius is so small that the escape velocity exceeds the speed of light ...
Stages 7 to 9 - Sun
... Off the Main Sequence - The Evolution of a Sun-like Star Stages 7 - 9 While on the main sequence, the star is burning hydrogen. It’s luminosity is determined by the stars mass. The most intense fusion is occurring at the center regions of the core (highest pressure and temperature). ...
... Off the Main Sequence - The Evolution of a Sun-like Star Stages 7 - 9 While on the main sequence, the star is burning hydrogen. It’s luminosity is determined by the stars mass. The most intense fusion is occurring at the center regions of the core (highest pressure and temperature). ...
Starlight and Atoms - School District of Clayton
... b. The upper layers of a star contain hot low-density gases that produce bright lines at precisely the same wavelengths as the dark lines, thus making them invisible. c. Hot hydrogen and helium gas in the interstellar medium produces bright lines to fill in the dark lines. d. The resolution of many ...
... b. The upper layers of a star contain hot low-density gases that produce bright lines at precisely the same wavelengths as the dark lines, thus making them invisible. c. Hot hydrogen and helium gas in the interstellar medium produces bright lines to fill in the dark lines. d. The resolution of many ...
Lyra
Lyra (/ˈlaɪərə/; Latin for lyre, from Greek λύρα) is a small constellation. It is one of 48 listed by the 2nd century astronomer Ptolemy, and is one of the 88 constellations recognized by the International Astronomical Union. Lyra was often represented on star maps as a vulture or an eagle carrying a lyre, and hence sometimes referred to as Aquila Cadens or Vultur Cadens. Beginning at the north, Lyra is bordered by Draco, Hercules, Vulpecula, and Cygnus. Lyra is visible from the northern hemisphere from spring through autumn, and nearly overhead, in temperate latitudes, during the summer months. From the southern hemisphere, it is visible low in the northern sky during the winter months.The lucida or brightest star—and one of the brightest stars in the sky—is the white main sequence star Vega, a corner of the Summer Triangle. Beta Lyrae is the prototype of a class of stars known as Beta Lyrae variables, binary stars so close to each other that they become egg-shaped and material flows from one to the other. Epsilon Lyrae, known informally as the Double Double, is a complex multiple star system. Lyra also hosts the Ring Nebula, the second-discovered and best-known planetary nebula.