Stellar evolution
... - First occurs in a runaway process: "the helium flash". Energy from fusion goes into re-expanding and cooling the core. This slows fusion, so star gets dimmer again. - Then stable He -> C burning. Still have H -> He shell burning surrounding it. ...
... - First occurs in a runaway process: "the helium flash". Energy from fusion goes into re-expanding and cooling the core. This slows fusion, so star gets dimmer again. - Then stable He -> C burning. Still have H -> He shell burning surrounding it. ...
Astronomy Library wk 7.cwk (WP)
... balmer lines. Reflection nebula: Starlight reflected off dust particles in the nebula. ...
... balmer lines. Reflection nebula: Starlight reflected off dust particles in the nebula. ...
Chemical evolution Observation of spiral and irregular galaxies
... Chemical evolution Observation of spiral and irregular galaxies show that the fraction of heavy elements varies with the fraction of the total mass which is in the form of gas: ...
... Chemical evolution Observation of spiral and irregular galaxies show that the fraction of heavy elements varies with the fraction of the total mass which is in the form of gas: ...
Section 25.2 Stellar Evolution
... remain in the stable main-sequence stage until they consume all their hydrogen fuel and collapse into a white dwarf. Death of Medium-Mass Stars Stars with masses similar to the sun evolve in essentially the same way as lowmass stars. During their collapse from red giants to white dwarfs, medium- ...
... remain in the stable main-sequence stage until they consume all their hydrogen fuel and collapse into a white dwarf. Death of Medium-Mass Stars Stars with masses similar to the sun evolve in essentially the same way as lowmass stars. During their collapse from red giants to white dwarfs, medium- ...
Planetarium Key Points
... The stars seem numberless and there are actually more than 2 billions of stars in the system we live in (Milky Way), but only 3000 stars are visible at naked eye What we see is NOT what it is actually, the response of our eye is logarithmic not linear All celestial objects seem at the same dis ...
... The stars seem numberless and there are actually more than 2 billions of stars in the system we live in (Milky Way), but only 3000 stars are visible at naked eye What we see is NOT what it is actually, the response of our eye is logarithmic not linear All celestial objects seem at the same dis ...
Lecture 10 - University of Minnesota
... forming cloud varies with density. Following these examples (especially the ones on page 533), figure out how dense the could would have to be to form a single, 1 solar mass star. What does this say about why stars usually form in clusters? ...
... forming cloud varies with density. Following these examples (especially the ones on page 533), figure out how dense the could would have to be to form a single, 1 solar mass star. What does this say about why stars usually form in clusters? ...
Where Is Everybody? - Center for Peripheral Studies
... Lee Drummond is director of the Center for Peripheral Studies, P O Box 477, Palm Springs CA 92262. Ideas previewed in this essay are developed at greater length in Drummond’s 1996 book, American Dreamtime: A Cultural Analysis of Popular Movies, and Their Implications for a Science of Humanity (Lanha ...
... Lee Drummond is director of the Center for Peripheral Studies, P O Box 477, Palm Springs CA 92262. Ideas previewed in this essay are developed at greater length in Drummond’s 1996 book, American Dreamtime: A Cultural Analysis of Popular Movies, and Their Implications for a Science of Humanity (Lanha ...
intropig
... where D is the optical density of the photopigment. (Thus, when D is low the normalized absorbance and absorbtance spectra are the same shape.) To compare an absorbance spectrum with a corneally-measured human spectral sensitivity, requires several steps and assumptions. First, we must know the effe ...
... where D is the optical density of the photopigment. (Thus, when D is low the normalized absorbance and absorbtance spectra are the same shape.) To compare an absorbance spectrum with a corneally-measured human spectral sensitivity, requires several steps and assumptions. First, we must know the effe ...
Amie Bickert - ColonialAcademyScience
... White dwarf: blue-white core of the star that is left behind cools forms this. Supernovas: an explosion of a suergiant Neutron star: the remains of high-mass stars. Black holes- an object with gravity so strong that nothing, not even light, can escape. Guided Practice: T. and Ss. read se ...
... White dwarf: blue-white core of the star that is left behind cools forms this. Supernovas: an explosion of a suergiant Neutron star: the remains of high-mass stars. Black holes- an object with gravity so strong that nothing, not even light, can escape. Guided Practice: T. and Ss. read se ...
Chapter 2 Observing the Electromagnetic Spectrum
... was launched into low Earth orbit on November 13th, 1978 and operated until April, 1981. It was the first X-ray mission to use focusing optics with imaging detectors and produce angular resolution of a few arc seconds3 ( ′′ ) and a field-of-view of tens of arc minutes ( ′ ). The Röntgen Observatory ...
... was launched into low Earth orbit on November 13th, 1978 and operated until April, 1981. It was the first X-ray mission to use focusing optics with imaging detectors and produce angular resolution of a few arc seconds3 ( ′′ ) and a field-of-view of tens of arc minutes ( ′ ). The Röntgen Observatory ...
o Lecturer: Dr. Peter Gallagher Email:
... o Bohr model was a major step toward understanding the quantum theory of the atom - not in fact a correct description of the nature of electron orbits. o Some of the shortcomings of the model are: 1. Fails describe why certain spectral lines are brighter than others => no mechanism for calculati ...
... o Bohr model was a major step toward understanding the quantum theory of the atom - not in fact a correct description of the nature of electron orbits. o Some of the shortcomings of the model are: 1. Fails describe why certain spectral lines are brighter than others => no mechanism for calculati ...
Wilmslow Guild Lecture 2008
... one Cepheid, all distances could be known. By using the Doppler effect in conjunction with Cepheid behaviour, it was for the first time possible to establish absolute distances and the size our galaxy. Many astronomers were involved in this process, and the final shape and distribution emerged in th ...
... one Cepheid, all distances could be known. By using the Doppler effect in conjunction with Cepheid behaviour, it was for the first time possible to establish absolute distances and the size our galaxy. Many astronomers were involved in this process, and the final shape and distribution emerged in th ...
Supernovae: Heavy Elements
... • The pressure of these neutrinos causes part of the imploding core to rebound • This rebound comes in the form of a shockwave, which rips through the still collapsing outer core • The collapsing outer shell is met by the shockwave and then by a rarefaction wave and is ejected back into space in a c ...
... • The pressure of these neutrinos causes part of the imploding core to rebound • This rebound comes in the form of a shockwave, which rips through the still collapsing outer core • The collapsing outer shell is met by the shockwave and then by a rarefaction wave and is ejected back into space in a c ...
Cepheid variable stars
... variations are caused by changes in the area and temperature of the star’s surface layers. Recent evidence suggests that all stars pulsate (if we measure them carefully enough), although the presence of concentrated populations of pulsating stars on the HR diagram implies that pulsations are more im ...
... variations are caused by changes in the area and temperature of the star’s surface layers. Recent evidence suggests that all stars pulsate (if we measure them carefully enough), although the presence of concentrated populations of pulsating stars on the HR diagram implies that pulsations are more im ...
Star Formation
... • marks the Sun’s outer boundary (500 km) • photons emitted into space (“light sphere”) ...
... • marks the Sun’s outer boundary (500 km) • photons emitted into space (“light sphere”) ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.