Ch. 5 Notes: Electrons in Atoms Big Idea: The Atoms of each
... a. Rutherford’s model of the atom did not explain how the electrons are arranged in the space around the nucleus. b. Rutherford’s model of the atom did not explain why the negatively charged electrons were not pulled into the positively charged nucleus. c. Rutherford’s model did not account for the ...
... a. Rutherford’s model of the atom did not explain how the electrons are arranged in the space around the nucleus. b. Rutherford’s model of the atom did not explain why the negatively charged electrons were not pulled into the positively charged nucleus. c. Rutherford’s model did not account for the ...
Key Areas covered
... Light and temperature • We can see that the temperature of an object affects the light it gives off. • This means that the temperature of an object is linked to both the frequency and wavelength of the light it emits. • A graph of intensity versus wavelength has a characteristic shape and can be sh ...
... Light and temperature • We can see that the temperature of an object affects the light it gives off. • This means that the temperature of an object is linked to both the frequency and wavelength of the light it emits. • A graph of intensity versus wavelength has a characteristic shape and can be sh ...
Rachel Henning
... 1. What is the expected fate of our sun? What happens to stars that are much more massive than our sun? In about 5 billion years, the hydrogen in the center of the Sun will start to run out. The helium will get squeezed. This will speed up the hydrogen burning. Our star will slowly puff into a red g ...
... 1. What is the expected fate of our sun? What happens to stars that are much more massive than our sun? In about 5 billion years, the hydrogen in the center of the Sun will start to run out. The helium will get squeezed. This will speed up the hydrogen burning. Our star will slowly puff into a red g ...
Life Cycle of Stars Flipbook Assignment
... 4. What happens that initiates the birth of a star? 5. Explain what happens in nuclear fusion? 6. What is going to happen to our Sun’s magnitude and temperature when it goes to its next stage? 7. What is the final stage of our Sun’s life? 8. What will happen to our Sun’s magnitude and temperature wh ...
... 4. What happens that initiates the birth of a star? 5. Explain what happens in nuclear fusion? 6. What is going to happen to our Sun’s magnitude and temperature when it goes to its next stage? 7. What is the final stage of our Sun’s life? 8. What will happen to our Sun’s magnitude and temperature wh ...
Galaxy Clusters
... Galaxies are the basic visible building blocks of the Universe. They are rarely found in isolation, but rather in sparse groups – sort of galactic urban sprawl. But occasional dense concentrations are found. The galaxies in these “Compact Groups” show dramatic differences in the way they evolve and ...
... Galaxies are the basic visible building blocks of the Universe. They are rarely found in isolation, but rather in sparse groups – sort of galactic urban sprawl. But occasional dense concentrations are found. The galaxies in these “Compact Groups” show dramatic differences in the way they evolve and ...
Stars - Red, Blue, Old, New pt.2
... Spitzer Space Telescope • Looks at the infrared with cameras and spectrographs. • Infrared radiation is “heat: can see through the dust much better than in optical ...
... Spitzer Space Telescope • Looks at the infrared with cameras and spectrographs. • Infrared radiation is “heat: can see through the dust much better than in optical ...
4-1. 1 - Riverside Local Schools
... 8. CONTINUOUS SPECTRUM is the spectrum produced when white light is passed through a prism. 9. LINE-EMISSION SPECTRUM of light is a series of specific wavelengths (or bands) of emitted light resulting from atoms loosing energy in the form of a photon…not a continuous spectrum 10. Additional series o ...
... 8. CONTINUOUS SPECTRUM is the spectrum produced when white light is passed through a prism. 9. LINE-EMISSION SPECTRUM of light is a series of specific wavelengths (or bands) of emitted light resulting from atoms loosing energy in the form of a photon…not a continuous spectrum 10. Additional series o ...
Constellations & Stars - Toms River Regional Schools :: Home
... • The Milky Way belongs to a group or cluster of galaxies called the local ...
... • The Milky Way belongs to a group or cluster of galaxies called the local ...
PSCI 1414 General Astronomy
... • Astronomical unit (AU) – The average distance between the Earth and the Sun ...
... • Astronomical unit (AU) – The average distance between the Earth and the Sun ...
Marcelo Borges Fernandes1, Michaela Kraus2, Jiri Kubát2
... and also a strong near or mid-infrared excess due to hot circumstellar dust. Based on Lamers et al. (1998), there are different types of objects presenting the B[e] phenomenon: pre-main sequence HAeBe stars, compact planetary nebula, symbiotic objects, hot supergiants – the most popular class with c ...
... and also a strong near or mid-infrared excess due to hot circumstellar dust. Based on Lamers et al. (1998), there are different types of objects presenting the B[e] phenomenon: pre-main sequence HAeBe stars, compact planetary nebula, symbiotic objects, hot supergiants – the most popular class with c ...
introduction to atomic structure
... Bohr’s Postulates: •Electron moves in circular orbits around the nucleus. •Electron can possess only certain energy values corresponding to the orbit. •Electron can “jump” from one orbit to another, the energy difference will be emitted or absorbed in the form of light quanta. ...
... Bohr’s Postulates: •Electron moves in circular orbits around the nucleus. •Electron can possess only certain energy values corresponding to the orbit. •Electron can “jump” from one orbit to another, the energy difference will be emitted or absorbed in the form of light quanta. ...
English - Cosmos
... The Sun is a star just like any other. We see stars as shiny dots because they are very far away from us. From Earth, what can we find out about stars? At first glance, we can see that stars’ colour is one of their properties. The hotter a star’s surface is, the bluer it will be. And the coldest, th ...
... The Sun is a star just like any other. We see stars as shiny dots because they are very far away from us. From Earth, what can we find out about stars? At first glance, we can see that stars’ colour is one of their properties. The hotter a star’s surface is, the bluer it will be. And the coldest, th ...
NORTH STAR PEOPLE
... arrow, is the spot that marks the center of our own galaxy, the Milky Way. The view towards the south is the most dazzling, interesting and inspiring view. If you turn around and face the north you will see a relatively dark sky. No really bright stars shine there, few interesting nebulae or galaxie ...
... arrow, is the spot that marks the center of our own galaxy, the Milky Way. The view towards the south is the most dazzling, interesting and inspiring view. If you turn around and face the north you will see a relatively dark sky. No really bright stars shine there, few interesting nebulae or galaxie ...
M - ASTRONOMY GROUP – University of St Andrews
... • MW + M31 dominate the light and mass • M31 is approaching us at about 85 km/s • Collision expected in ~10 billion years ! • LG will eventually merge to form one giant ...
... • MW + M31 dominate the light and mass • M31 is approaching us at about 85 km/s • Collision expected in ~10 billion years ! • LG will eventually merge to form one giant ...
Animated Planets PowerPoint Presentation
... LT: Understand comet make-up, properties, Vocab.: 1. comet nucleus 2. Halley’s comet 3. “dirty snowball” Agenda: Comet Notes ...
... LT: Understand comet make-up, properties, Vocab.: 1. comet nucleus 2. Halley’s comet 3. “dirty snowball” Agenda: Comet Notes ...
ASTRONOMY 157 – Stars and Galaxies - Syllabus
... Quasars; galactic BH formation; Lyman alpha forest Recommended Text: Web references Grade Structure: Midterms (2) - 30% each Final exam - 40% Exam Format: Eight to twelve questions will be posted on Bb several weeks before each test. Two of them will appear on the test. Each question will have five ...
... Quasars; galactic BH formation; Lyman alpha forest Recommended Text: Web references Grade Structure: Midterms (2) - 30% each Final exam - 40% Exam Format: Eight to twelve questions will be posted on Bb several weeks before each test. Two of them will appear on the test. Each question will have five ...
Exercise G1: Our Home Galaxy, the Milky Way
... Question 3: The Sun is moving with a velocity of about 220 km/sec in its orbit about the galactic center. Using your answer from Question 2, what is the approximate time required for the Sun (and the entire Solar System) to complete one orbit of the galactic center? a. 115 million years b. 230 m ...
... Question 3: The Sun is moving with a velocity of about 220 km/sec in its orbit about the galactic center. Using your answer from Question 2, what is the approximate time required for the Sun (and the entire Solar System) to complete one orbit of the galactic center? a. 115 million years b. 230 m ...
Introduction to Electromagnetism
... We derived the Schwarzschild radius for a black hole; we weighed Jupiter and the Sun using orbital satellites, and we discovered dark matter in Galaxies from non-Keplerian velocity curves 2.4 The Virial Theorem: E = U/2 in a central field. ...
... We derived the Schwarzschild radius for a black hole; we weighed Jupiter and the Sun using orbital satellites, and we discovered dark matter in Galaxies from non-Keplerian velocity curves 2.4 The Virial Theorem: E = U/2 in a central field. ...
A Tale of Star and Planet Formation
... Our Sun is a single star, but half of all Sun-like stars are found to be in multiple systems (twins, triplets, quads). Models of star formation have trouble predicting exactly how these systems are made. ...
... Our Sun is a single star, but half of all Sun-like stars are found to be in multiple systems (twins, triplets, quads). Models of star formation have trouble predicting exactly how these systems are made. ...
proposed research projects for pparc gemini studentships
... This project aims at determining the main physical drivers governing the formation of S0 galaxies, and their dependency on galaxy mass. To this end, we propose a spectral study of a large sample of lenticular systems to establish the links between the properties of their stellar populations (ages an ...
... This project aims at determining the main physical drivers governing the formation of S0 galaxies, and their dependency on galaxy mass. To this end, we propose a spectral study of a large sample of lenticular systems to establish the links between the properties of their stellar populations (ages an ...
The sodium D-lines Why and What are D
... The Fraunhofer lines are a set of spectral lines named for the German physicist Joseph von Fraunhofer (1787– 1826). The lines were originally observed as dark features (absorption lines) in the optical spectrum of the Sun. He labeled the lines with letters from A to K. ...
... The Fraunhofer lines are a set of spectral lines named for the German physicist Joseph von Fraunhofer (1787– 1826). The lines were originally observed as dark features (absorption lines) in the optical spectrum of the Sun. He labeled the lines with letters from A to K. ...
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.