Interstellar Gas
... In the atmosphere of a star, individual atoms are rushing randomly to and fro at various speeds – some towards us, some away – because the gas is hot. Thanks to the Doppler shift, each of them absorbs light coming out of the star’s interior at a slightly different wavelength. This means that the abs ...
... In the atmosphere of a star, individual atoms are rushing randomly to and fro at various speeds – some towards us, some away – because the gas is hot. Thanks to the Doppler shift, each of them absorbs light coming out of the star’s interior at a slightly different wavelength. This means that the abs ...
The Interstellar Medium (ISM) Part II: Interstellar Gas
... In the atmosphere of a star, individual atoms are rushing randomly to and fro at various speeds – some towards us, some away – because the gas is hot. Thanks to the Doppler shift, each of them absorbs light coming out of the star’s interior at a slightly different wavelength. This means that the abs ...
... In the atmosphere of a star, individual atoms are rushing randomly to and fro at various speeds – some towards us, some away – because the gas is hot. Thanks to the Doppler shift, each of them absorbs light coming out of the star’s interior at a slightly different wavelength. This means that the abs ...
Spectroscopic Investigation of Companion Stars in Herbig
... Stars were chosen to be the known binary companion to a Herbig star, with a binary separation greater than 0.8 arcseconds to avoid any contamination from the primary star. Data was collected using the Gemini South GNIRS instrument (PI Rodgers).Two types of spectral measurements were made, high resol ...
... Stars were chosen to be the known binary companion to a Herbig star, with a binary separation greater than 0.8 arcseconds to avoid any contamination from the primary star. Data was collected using the Gemini South GNIRS instrument (PI Rodgers).Two types of spectral measurements were made, high resol ...
Study Guide for 3RD Astronomy Exam
... State or identify what additional information can be obtained from and eclipsing binaries besides the combined mass of the stars. Determine the combined mass of a binary star system using ...
... State or identify what additional information can be obtained from and eclipsing binaries besides the combined mass of the stars. Determine the combined mass of a binary star system using ...
Guess The Spectra!!
... Sun, but is a different color! The color difference is due to temperature. Rigel is 2x as hot as the Sun so it appears blue! ...
... Sun, but is a different color! The color difference is due to temperature. Rigel is 2x as hot as the Sun so it appears blue! ...
The Life Cycle of a Star and the Hertzsprung
... stars of different ages and in different stages, all at the same time. It is also a great tool to check your understanding of the star life cycle. 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 ...
... stars of different ages and in different stages, all at the same time. It is also a great tool to check your understanding of the star life cycle. 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 ...
Review Packet
... Every 6 points that are correct, you will earn 1 extra credit point on the exam. Up to 18 points are available. The Life Cycle of Stars Section One – Sequencing (6 points) The stages below are not in the right order. Number the stages in the correct order. _____ The star begins to run out of fuel an ...
... Every 6 points that are correct, you will earn 1 extra credit point on the exam. Up to 18 points are available. The Life Cycle of Stars Section One – Sequencing (6 points) The stages below are not in the right order. Number the stages in the correct order. _____ The star begins to run out of fuel an ...
Stars
... distance of each star from the center of mass yields the ratio of the masses. •The ratio and sum provide each mass individually. ...
... distance of each star from the center of mass yields the ratio of the masses. •The ratio and sum provide each mass individually. ...
Lecture 11: The Internal Structure of Stars
... very small volume of space) can have the same energy. Adding more particles at the same energy (=degenerate particles) is not allowed. If there are any more particles in the box, they must be moving. Particles moving quickly=high pressure Different kind of pressure than ideal gas pressure Pressure d ...
... very small volume of space) can have the same energy. Adding more particles at the same energy (=degenerate particles) is not allowed. If there are any more particles in the box, they must be moving. Particles moving quickly=high pressure Different kind of pressure than ideal gas pressure Pressure d ...
HW9_Answers
... cool to a certain temperature. There are no white dwarf stars cooler than about spectral type K. This is because there hasn’t been enough time for them to cool any further since the start of the universe. Knowing the cooling rate, and the cutoff in temperature for the white dwarfs, gives an age for ...
... cool to a certain temperature. There are no white dwarf stars cooler than about spectral type K. This is because there hasn’t been enough time for them to cool any further since the start of the universe. Knowing the cooling rate, and the cutoff in temperature for the white dwarfs, gives an age for ...
HW #9 Answers (Due 10/28)
... cool to a certain temperature. There are no white dwarf stars cooler than about spectral type K. This is because there hasn’t been enough time for them to cool any further since the start of the universe. Knowing the cooling rate, and the cutoff in temperature for the white dwarfs, gives an age for ...
... cool to a certain temperature. There are no white dwarf stars cooler than about spectral type K. This is because there hasn’t been enough time for them to cool any further since the start of the universe. Knowing the cooling rate, and the cutoff in temperature for the white dwarfs, gives an age for ...
Astronomy Facts
... The sun is 1.4 million km across (110 times the earth), and over 150 million km away (500 light seconds) The largest stars (eg: Betelgeuse, Antares) are over 400 million km across (more than 300 times the diameter of the Sun) The brightest stars are over 10,000 times brighter than the sun. The dista ...
... The sun is 1.4 million km across (110 times the earth), and over 150 million km away (500 light seconds) The largest stars (eg: Betelgeuse, Antares) are over 400 million km across (more than 300 times the diameter of the Sun) The brightest stars are over 10,000 times brighter than the sun. The dista ...
Answers to Coursebook questions – Chapter E2
... groupings of stars. Main sequence stars occupy a strip going diagonally down from top left to bottom right, red giants are in the top left part of the diagram and white dwarfs are at the bottom left. ...
... groupings of stars. Main sequence stars occupy a strip going diagonally down from top left to bottom right, red giants are in the top left part of the diagram and white dwarfs are at the bottom left. ...
Evolution of High
... The degenerate pressure of electrons in the inert iron core cannot support the star against the pull of gravity only briefly, due to the high mass of the star. In an instant, electrons are force to combine with the protons in the iron nuclei to form neutrons, releasing neutrinos in the process. • Th ...
... The degenerate pressure of electrons in the inert iron core cannot support the star against the pull of gravity only briefly, due to the high mass of the star. In an instant, electrons are force to combine with the protons in the iron nuclei to form neutrons, releasing neutrinos in the process. • Th ...
The correct answers are written in bold, italic and underlined. The
... fraction of the initial ionized hydrogen atom? • About 100% ...
... fraction of the initial ionized hydrogen atom? • About 100% ...
File
... constellation of Cygnus. The angular difference was found to be 0.292 arcseconds. This gives a distance of 3.48 pc, or 11.36 light years ...
... constellation of Cygnus. The angular difference was found to be 0.292 arcseconds. This gives a distance of 3.48 pc, or 11.36 light years ...
galctr
... constancy of S2 in K band => disk either optically thin at K or large inner hole L band excess possibly interpreted as reprocessing from disk Overall conclusion: no current cold disk is present ...
... constancy of S2 in K band => disk either optically thin at K or large inner hole L band excess possibly interpreted as reprocessing from disk Overall conclusion: no current cold disk is present ...
Introduction to the HR Diagram
... contract once again, and this time the temperature becomes hot enough to start helium burning. The outer layers expand even further, becoming cooler and redder. Giant stars fuse elements up to carbon. Most of these stars go through a Mira variable instability strip with a periodic light curve of ~80 ...
... contract once again, and this time the temperature becomes hot enough to start helium burning. The outer layers expand even further, becoming cooler and redder. Giant stars fuse elements up to carbon. Most of these stars go through a Mira variable instability strip with a periodic light curve of ~80 ...