Support worksheet – Topic 3 Questions
... Suggest why the stellar parallax method is limited to distances of about 300 pc for Earth-based telescopes but can be extended to 1000 pc for satellite-based telescopes. ...
... Suggest why the stellar parallax method is limited to distances of about 300 pc for Earth-based telescopes but can be extended to 1000 pc for satellite-based telescopes. ...
DR 19.2 - Cobb Learning
... ______ 21. stars with low mass, low temperature, and low absolute magnitude ______ 22. small hot stars that are dimmer than the sun ______ 23. high-temperature stars that quickly use up their hydrogen ______ 24. cool stars with absolute magnitude ______ 25. stars in the band that runs along the midd ...
... ______ 21. stars with low mass, low temperature, and low absolute magnitude ______ 22. small hot stars that are dimmer than the sun ______ 23. high-temperature stars that quickly use up their hydrogen ______ 24. cool stars with absolute magnitude ______ 25. stars in the band that runs along the midd ...
Where Do Chemical Elements Come From?
... the collapse that the very special conditions of pressure and temperature exist in the supernova that allow for the formation of elements heavier than iron. The newly created elements are ejected into the interstellar dust and gas surrounding the star. “The amount of elements released through a supe ...
... the collapse that the very special conditions of pressure and temperature exist in the supernova that allow for the formation of elements heavier than iron. The newly created elements are ejected into the interstellar dust and gas surrounding the star. “The amount of elements released through a supe ...
TTh HW06 key
... 1. Thermonuclear fusion reactions in the core of the Sun convert four hydrogen nuclei into one helium nucleus. The helium nucleus has A) less mass than the four hydrogen nuclei. B) the same mass as the four hydrogen nuclei. C) an undetermined amount of mass that depends on the temperature at which t ...
... 1. Thermonuclear fusion reactions in the core of the Sun convert four hydrogen nuclei into one helium nucleus. The helium nucleus has A) less mass than the four hydrogen nuclei. B) the same mass as the four hydrogen nuclei. C) an undetermined amount of mass that depends on the temperature at which t ...
F03HW12
... the star clusters show us that when giants and supergiants are present in the clusters, there are few if any massive stars (O and B stars) on the main sequence. We can take models of many different masses of stars and determine what a cluster should look like after a given time. We can then compare ...
... the star clusters show us that when giants and supergiants are present in the clusters, there are few if any massive stars (O and B stars) on the main sequence. We can take models of many different masses of stars and determine what a cluster should look like after a given time. We can then compare ...
Review Questions for Chp 2
... 7. Identify 3 things the H-R diagram indicates about stars. 8. What are the three types of galaxies? 9. Why are globular star clusters different from open star clusters? 10. What is a quasar and why is it so important? 11. How did the universe form? Pick the theory that is supported with the most ev ...
... 7. Identify 3 things the H-R diagram indicates about stars. 8. What are the three types of galaxies? 9. Why are globular star clusters different from open star clusters? 10. What is a quasar and why is it so important? 11. How did the universe form? Pick the theory that is supported with the most ev ...
05spectralclasses
... Classification of Stellar Spectra Late 1800s: first high-quality spectral measurements of stars What are the main features – and how to classify them? ...
... Classification of Stellar Spectra Late 1800s: first high-quality spectral measurements of stars What are the main features – and how to classify them? ...
Space Study Guide
... Smaller stars that are equivalent to 0-8 of our suns mass will enter the white dwarf stage where the star appears smaller and shines brightly. When its fuel runs out it becomes dark cold and is called a black dwarf. Medium sized stars that are 8-20 of our solar masses will go from a red giant stage ...
... Smaller stars that are equivalent to 0-8 of our suns mass will enter the white dwarf stage where the star appears smaller and shines brightly. When its fuel runs out it becomes dark cold and is called a black dwarf. Medium sized stars that are 8-20 of our solar masses will go from a red giant stage ...
2nd Semester Exam Study Guide
... moving away from the Milky Way galaxy. 7. After the Big Bang occurred, many atoms of hydrogen and helium formed when temperatures decreased and gravitational attractions lead to the formation of trillions of stars. 8. The peak wavelength for objects depends on the intensity of light given off at a c ...
... moving away from the Milky Way galaxy. 7. After the Big Bang occurred, many atoms of hydrogen and helium formed when temperatures decreased and gravitational attractions lead to the formation of trillions of stars. 8. The peak wavelength for objects depends on the intensity of light given off at a c ...
November 2005 - Otterbein University
... • Core contains 25% of the star’s mass and continues to shrink • Strong stellar winds eject up to 30% of stars mass from surface • Duration: 100,000 years • Temperature: 100 106 K (core) to 4000 K (surface) • Size ~ 70 Suns (orbit of ...
... • Core contains 25% of the star’s mass and continues to shrink • Strong stellar winds eject up to 30% of stars mass from surface • Duration: 100,000 years • Temperature: 100 106 K (core) to 4000 K (surface) • Size ~ 70 Suns (orbit of ...
Stars
... star really looks from Earth. The farther away from us, the dimmer the star looks. • Absolute Magnitude – How bright the star really is. If all stars were the same distance from us, how bright would it look compared to the other ...
... star really looks from Earth. The farther away from us, the dimmer the star looks. • Absolute Magnitude – How bright the star really is. If all stars were the same distance from us, how bright would it look compared to the other ...
The birth and life of stars
... star becomes unstable and begins to pulsate. RR Lyrae variables are low-mass, pulsating variables with short periods. Cepheid variables are high-mass, pulsating variables exhibiting a regular relationship between the period of pulsation and luminosity. Mass can be transferred from one star to an ...
... star becomes unstable and begins to pulsate. RR Lyrae variables are low-mass, pulsating variables with short periods. Cepheid variables are high-mass, pulsating variables exhibiting a regular relationship between the period of pulsation and luminosity. Mass can be transferred from one star to an ...
types of stars, luminosity, and brightness
... intrinsic energy per sec that a star radiates and does not depend on our distance from the star. 7. Stars are classified by temperature and luminosity. 8. Supergiants are the most luminous and white dwarfs are the least luminous. 9. The main characteristic of main sequence stars is that they have hy ...
... intrinsic energy per sec that a star radiates and does not depend on our distance from the star. 7. Stars are classified by temperature and luminosity. 8. Supergiants are the most luminous and white dwarfs are the least luminous. 9. The main characteristic of main sequence stars is that they have hy ...
Stellar Spectra
... • Almost all stars show a “continuum” spectrum with “absorption” lines. • Some stars show “emission” lines. – All stars do not have the same spectrum! • Interstellar clouds show a continuum with emission lines ...
... • Almost all stars show a “continuum” spectrum with “absorption” lines. • Some stars show “emission” lines. – All stars do not have the same spectrum! • Interstellar clouds show a continuum with emission lines ...
File
... 10. The region of the Hertzsprung-Russell diagram that most stars fall within is the ______________________ . 11. A graph of stars showing surface temperature on the x-axis and absolute brightness on the y-axis is a(n) ________________________ . 12. ______________________ is often used to determine ...
... 10. The region of the Hertzsprung-Russell diagram that most stars fall within is the ______________________ . 11. A graph of stars showing surface temperature on the x-axis and absolute brightness on the y-axis is a(n) ________________________ . 12. ______________________ is often used to determine ...
death_high_mass
... Helium gone in the core • Helium fusion rate is much faster than the Hydrogen fusion rate was. Within a few hundred million years the supply is gone in the core. • The core once again shrinks, releasing gravitational potential energy. • The material in a shell closest to the core begins to fuse hel ...
... Helium gone in the core • Helium fusion rate is much faster than the Hydrogen fusion rate was. Within a few hundred million years the supply is gone in the core. • The core once again shrinks, releasing gravitational potential energy. • The material in a shell closest to the core begins to fuse hel ...
Chapter 25 PowerPoint
... over the next few hundred million years, it will fuse hydrogen in a spherical shell around the center of the star. In this phase, the Sun will turn into a red giant. The center of the Sun will not be hot enough to fuse helium, and will be surrounded by a layer where there is hydrogen still burning. ...
... over the next few hundred million years, it will fuse hydrogen in a spherical shell around the center of the star. In this phase, the Sun will turn into a red giant. The center of the Sun will not be hot enough to fuse helium, and will be surrounded by a layer where there is hydrogen still burning. ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.