Basic Astronomy Note - Mr. Dewey – Grade 7/8
... Basic Astronomy Note When you look up at the night sky, all of the stars you see are suns - many of which are much larger than our sun – but so incredibly far away they appear to us as tiny points of light. Stars are bodies of gas molecules (hydrogen atoms compressing and fusing into helium). This i ...
... Basic Astronomy Note When you look up at the night sky, all of the stars you see are suns - many of which are much larger than our sun – but so incredibly far away they appear to us as tiny points of light. Stars are bodies of gas molecules (hydrogen atoms compressing and fusing into helium). This i ...
Extracting science from surveys of our Galaxy
... There’s a huge and rapidly growing volume of survey data for MW ¤CDM does not currently predict the structure of the MW Key observables (,¹) are far removed from quantities of physical interest Errors in s corrupt estimates of all physical quantities Inversion of data to physical model ill-advised ...
... There’s a huge and rapidly growing volume of survey data for MW ¤CDM does not currently predict the structure of the MW Key observables (,¹) are far removed from quantities of physical interest Errors in s corrupt estimates of all physical quantities Inversion of data to physical model ill-advised ...
Stellar Luminosity and Mass Functions * * * * * History and
... Massive stars have short lifetimes Suppose we observe the luminosity function of an old cluster. There are no very luminous main sequence stars. But this does not mean that the IMF of the cluster had zero massive stars, only that such stars have ended their main sequence lifetimes. More generally, ...
... Massive stars have short lifetimes Suppose we observe the luminosity function of an old cluster. There are no very luminous main sequence stars. But this does not mean that the IMF of the cluster had zero massive stars, only that such stars have ended their main sequence lifetimes. More generally, ...
SNC 1D1 Space Unit Review Answers How long does it take the
... 24. Name and describe the predominant scientific theory on how the universe was formed. -Big Bang Theory: 14 billion years ago, everything in the Universe existed in a single fixed mass that was hot and dense. -Suddenly, 13.8 billion years ago, there was a tremendous explosion that started the expan ...
... 24. Name and describe the predominant scientific theory on how the universe was formed. -Big Bang Theory: 14 billion years ago, everything in the Universe existed in a single fixed mass that was hot and dense. -Suddenly, 13.8 billion years ago, there was a tremendous explosion that started the expan ...
presentation format
... If objects have transverse velocity, they will fall around other object, i.e., they will orbit around other objects To understand why the planets orbit the Sun rather than fall into it, we need to understand how they got their initial transverse velocity. Origin of the Solar System ...
... If objects have transverse velocity, they will fall around other object, i.e., they will orbit around other objects To understand why the planets orbit the Sun rather than fall into it, we need to understand how they got their initial transverse velocity. Origin of the Solar System ...
Calculating Main Sequence Lifetimes
... begin new fusion reactions involving the burning of Helium, Carbon, Oxygen, Magnesium and Neon. A star with a mass greater than 10 solar masses can develop thermonuclear reactions until it creates Iron. This will cause an ending to its life in a supernova type II. The luminosity (L) of a star is the ...
... begin new fusion reactions involving the burning of Helium, Carbon, Oxygen, Magnesium and Neon. A star with a mass greater than 10 solar masses can develop thermonuclear reactions until it creates Iron. This will cause an ending to its life in a supernova type II. The luminosity (L) of a star is the ...
Chapter 7 Lect. 1
... B. Characteristics of Light 1. Wavelength = distance between two peaks in a wave a. l (lambda) is the symbol b. Meters = m is the unit 2. Frequency = number of complete waves passing a given point per second a. n (nu) is the symbol b. Hertz = Hz = s-1 is the unit 3. Amplitude = A = measure of the i ...
... B. Characteristics of Light 1. Wavelength = distance between two peaks in a wave a. l (lambda) is the symbol b. Meters = m is the unit 2. Frequency = number of complete waves passing a given point per second a. n (nu) is the symbol b. Hertz = Hz = s-1 is the unit 3. Amplitude = A = measure of the i ...
Lectures 3-5 - U of L Class Index
... If an atom is struck by a photon that has enough energy, it will absorb the photon. This puts the atom into an excited state. (An atom that has absorbed no energy from external sources is said to be in its ground state.) ...
... If an atom is struck by a photon that has enough energy, it will absorb the photon. This puts the atom into an excited state. (An atom that has absorbed no energy from external sources is said to be in its ground state.) ...
The Birdseed Galaxy - Secondary Education
... way out from the center of our Galaxy. So where is that in the U.S.? Maybe over the Rocky Mountains. What else in North America is half-way from the center? (Students could make measurements on a map of North America, perhaps one they print out from the Web.) 3. The Number of Stars in the Galaxy Our ...
... way out from the center of our Galaxy. So where is that in the U.S.? Maybe over the Rocky Mountains. What else in North America is half-way from the center? (Students could make measurements on a map of North America, perhaps one they print out from the Web.) 3. The Number of Stars in the Galaxy Our ...
Lectures 3-5 - University of Lethbridge
... If an atom is struck by a photon that has enough energy, it will absorb the photon. This puts the atom into an excited state. (An atom that has absorbed no energy from external sources is said to be in its ground state.) ...
... If an atom is struck by a photon that has enough energy, it will absorb the photon. This puts the atom into an excited state. (An atom that has absorbed no energy from external sources is said to be in its ground state.) ...
Slide 1
... Formation of the Solar System Nebular Theory = sun and planets formed from a rotating disk of dust and gases. Planetesimals = small, irregular-shaped bodies that collided and clumped together to form the planets. ...
... Formation of the Solar System Nebular Theory = sun and planets formed from a rotating disk of dust and gases. Planetesimals = small, irregular-shaped bodies that collided and clumped together to form the planets. ...
Dark Matter Spiral Structure Basic Galaxy Morphology Disk Galaxy Rotation Curves:
... Passive " Actively star forming Red colors " Blue colors Hot gas " Cold gas and dust Old " Still forming High luminosity density " Low lum. dens. … etc. But, for example, masses, luminosities, sizes, etc., do not correlate well with the Hubble type: at every type there is a large spread in these fun ...
... Passive " Actively star forming Red colors " Blue colors Hot gas " Cold gas and dust Old " Still forming High luminosity density " Low lum. dens. … etc. But, for example, masses, luminosities, sizes, etc., do not correlate well with the Hubble type: at every type there is a large spread in these fun ...
Unit 4: Atoms and Nuclei
... (1) Bohr proposed that certain “magical” circular orbits existed, called “stationary states”, which did not radiate, and that electrons could only exist in these states, with radiation occurring when they made the transition from one to the other. (2) He also postulated that the frequency of the ra ...
... (1) Bohr proposed that certain “magical” circular orbits existed, called “stationary states”, which did not radiate, and that electrons could only exist in these states, with radiation occurring when they made the transition from one to the other. (2) He also postulated that the frequency of the ra ...
VISIT TO NORMAN LOCKYER OBSERVATORY IN SIDMOUTH
... To find it in the sky, follow the arc of the Plough's handle downwards to first find the orange star Arcturus and continue down to find the white, first magnitude star, Spica, in Virgo. Saturn, a little brighter than Spica, lies in Libra down to its lower left and will appear slightly yellow in colo ...
... To find it in the sky, follow the arc of the Plough's handle downwards to first find the orange star Arcturus and continue down to find the white, first magnitude star, Spica, in Virgo. Saturn, a little brighter than Spica, lies in Libra down to its lower left and will appear slightly yellow in colo ...
Star Fromation and ISM
... nuclear fusion begins. The protostar has become a star. The star continues to contract and increase in temperature, until it is in equilibrium. This is stage 7: the star has reached the main sequence and will remain there as long as it has hydrogen to fuse. ...
... nuclear fusion begins. The protostar has become a star. The star continues to contract and increase in temperature, until it is in equilibrium. This is stage 7: the star has reached the main sequence and will remain there as long as it has hydrogen to fuse. ...
the Contributed Poster
... the online homework. The question asked students to draw a graph similar to the one in the pretest. It also asked students to draw the graph for a light bulb emitting less total power, and to describe any differences between the graphs. The table below summarizes the exam results, as well as the pre ...
... the online homework. The question asked students to draw a graph similar to the one in the pretest. It also asked students to draw the graph for a light bulb emitting less total power, and to describe any differences between the graphs. The table below summarizes the exam results, as well as the pre ...
Life Before the Fall: Group Galaxy Evolution Prior to Cluster Assembly
... Relation of above quantities to local density and galaxy mass (Chandra, ACS, BVRJKs imaging, MIPS, spectroscopy) Ringberg Workshop - October 25, 2005 ...
... Relation of above quantities to local density and galaxy mass (Chandra, ACS, BVRJKs imaging, MIPS, spectroscopy) Ringberg Workshop - October 25, 2005 ...
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.