XI. Astronomy: Solar-System Debris and Comets
... b. The discrepancy probably wasn’t real: the wrong mass had been assumed for Neptune when predicting the orbit of Uranus. c. Thus, Pluto just happened to be in the predicted part of the sky! However, the discovery of Pluto remains a testament to Tombaugh’s skill and thoroughness: it was a very dot a ...
... b. The discrepancy probably wasn’t real: the wrong mass had been assumed for Neptune when predicting the orbit of Uranus. c. Thus, Pluto just happened to be in the predicted part of the sky! However, the discovery of Pluto remains a testament to Tombaugh’s skill and thoroughness: it was a very dot a ...
Chapter 1 Periods of Western Astronomy Prehistoric Astronomy
... • Because of the general east to west motion of objects in the sky, geocentric theories were developed to explain the motions • Eudoxus (400-347 B.C.) proposed a geocentric model in which each celestial object was mounted on its own revolving transparent sphere with its own separate tilt • The faste ...
... • Because of the general east to west motion of objects in the sky, geocentric theories were developed to explain the motions • Eudoxus (400-347 B.C.) proposed a geocentric model in which each celestial object was mounted on its own revolving transparent sphere with its own separate tilt • The faste ...
Document
... Hitting the Earth? • There may come a day when one of those asteroids drops out of orbit (maybe from a collision with another asteroid) and heads toward Earth. • If it is small enough, it will burn up in the atmosphere. • Larger ones (over 10 km across) will hit the surface of the planet. • Hundred ...
... Hitting the Earth? • There may come a day when one of those asteroids drops out of orbit (maybe from a collision with another asteroid) and heads toward Earth. • If it is small enough, it will burn up in the atmosphere. • Larger ones (over 10 km across) will hit the surface of the planet. • Hundred ...
Science 8 Name: Unit 2 Astronomy Date: Period: ______ Class
... the core undergoes a change. Atoms of H collide violently. During these collisions the nuclei of H atoms join together to produce He. This joining of atomic nuclei is called nuclear fusion. During nuclear fusion a certain amount of matter is lost. The He nuclei joined together have less mass than th ...
... the core undergoes a change. Atoms of H collide violently. During these collisions the nuclei of H atoms join together to produce He. This joining of atomic nuclei is called nuclear fusion. During nuclear fusion a certain amount of matter is lost. The He nuclei joined together have less mass than th ...
Outer Space
... suits. The Moon has no air or water. Plants and animals can’t live there either. Astronauts first landed on the Moon in 1969. After that, there were six more trips to the Moon. They brought back Moon rocks, which scientists are still studying. There are holes, or craters, all over the Moon’s surface ...
... suits. The Moon has no air or water. Plants and animals can’t live there either. Astronauts first landed on the Moon in 1969. After that, there were six more trips to the Moon. They brought back Moon rocks, which scientists are still studying. There are holes, or craters, all over the Moon’s surface ...
Introduction to Astronomy
... • Also faintly visible at other wavelengths • A few hundred are now known • What are they? Rapidly spinning neutron stars, whose strong magnetic fields accelerate plasma to produce the beam of radio waves ...
... • Also faintly visible at other wavelengths • A few hundred are now known • What are they? Rapidly spinning neutron stars, whose strong magnetic fields accelerate plasma to produce the beam of radio waves ...
Astro-Spectroscpy
... Structure of the Sun: Three Zones Core, Radiative, Convective • Energy is produced in the core via thermonuclear reactions and radiates out through the star • Radiation diffuses through the Radiative zone via lightmatter interactions • Convection occurs in the outermost regions before radiation eme ...
... Structure of the Sun: Three Zones Core, Radiative, Convective • Energy is produced in the core via thermonuclear reactions and radiates out through the star • Radiation diffuses through the Radiative zone via lightmatter interactions • Convection occurs in the outermost regions before radiation eme ...
Test#3
... 1. A measurement of the parallax of a star allows us directly to determine the star's a) rotation rate, b) temperature, c) distance, d) age 2. How much brighter would a star be if an observer moved from 3 to 1 parsec from the star? a) 3 times, b) 9 times, c) 27 times, d) 81 times 3. The difference b ...
... 1. A measurement of the parallax of a star allows us directly to determine the star's a) rotation rate, b) temperature, c) distance, d) age 2. How much brighter would a star be if an observer moved from 3 to 1 parsec from the star? a) 3 times, b) 9 times, c) 27 times, d) 81 times 3. The difference b ...
Answer Key Cloze
... Jupiter is composed mostly of gas. This enormous planet radiates twice as much heat as it absorbs from the Sun. It also has an extremely strong magnetic field. The planet is slightly flattened at its poles and it bulges out a bit at the equator. It takes Jupiter 9.8 Earth hours to revolve around its ...
... Jupiter is composed mostly of gas. This enormous planet radiates twice as much heat as it absorbs from the Sun. It also has an extremely strong magnetic field. The planet is slightly flattened at its poles and it bulges out a bit at the equator. It takes Jupiter 9.8 Earth hours to revolve around its ...
The Sun
... The sun creates energy by nuclear fusion in its core The visible surface of the Sun is called the photosphere A thin cool layer, the chromosphere, allows us to determine what the sun is made of A very thin but very hot outer layer is called the corona Convection in the sun is revealed by granulation ...
... The sun creates energy by nuclear fusion in its core The visible surface of the Sun is called the photosphere A thin cool layer, the chromosphere, allows us to determine what the sun is made of A very thin but very hot outer layer is called the corona Convection in the sun is revealed by granulation ...
Star - AUSD Blogs
... magnetic tape and the thousands of photographs we are carrying back to earth. Other scientists can interpret them as easily as I can, and I am not one who would condone that tampering with the truth which often gave my order a bad name in the olden days. The crew are already sufficiently depressed: ...
... magnetic tape and the thousands of photographs we are carrying back to earth. Other scientists can interpret them as easily as I can, and I am not one who would condone that tampering with the truth which often gave my order a bad name in the olden days. The crew are already sufficiently depressed: ...
general information on uranus
... Jupiter is the ____________________________________ in our solar system. This gas giant has a thick atmosphere, 39 known moons, and ______________________________. Its most prominent features are bands across its latitudes _____________________________________). Jupiter is composed ___________ ...
... Jupiter is the ____________________________________ in our solar system. This gas giant has a thick atmosphere, 39 known moons, and ______________________________. Its most prominent features are bands across its latitudes _____________________________________). Jupiter is composed ___________ ...
ph709-08-3b - Centre for Astrophysics and Planetary Science
... there's too little solid material in the vicinity to build protoplanet's core of 10 ME (applies to r~1 AU as well). ...
... there's too little solid material in the vicinity to build protoplanet's core of 10 ME (applies to r~1 AU as well). ...
Chapter 2 Astronomy Notes
... (2) A "dwarf planet" is a celestial body that: (a) is in orbit around the Sun, (b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, (c) has not cleared the neighbourhood around its orbit, and (d) is not a satell ...
... (2) A "dwarf planet" is a celestial body that: (a) is in orbit around the Sun, (b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, (c) has not cleared the neighbourhood around its orbit, and (d) is not a satell ...
Document
... This invisible force reaches into space to form the magnetosphere, protecting us from the solar wind. But the magnetic field is in a constant state of flux and is showing significant weakening and could even go into reverse. ...
... This invisible force reaches into space to form the magnetosphere, protecting us from the solar wind. But the magnetic field is in a constant state of flux and is showing significant weakening and could even go into reverse. ...
March 2011 - Sunderland Astronomical Society
... faster and faster as the distance shrinks. When each star’s rotation period on its axis is the same as its orbital period around the other, the pair effectively rotates as a single body in just 3 or 4 days. Then, watch out! Such fast spinning intensifies the magnetic dynamo inside each star. The sta ...
... faster and faster as the distance shrinks. When each star’s rotation period on its axis is the same as its orbital period around the other, the pair effectively rotates as a single body in just 3 or 4 days. Then, watch out! Such fast spinning intensifies the magnetic dynamo inside each star. The sta ...
Composition of the Sun
... lines of starlight to those of Earth’s elements, and identify the elements in the star’s atmosphere. Both hydrogen and helium occur in the sun. About 75% of the sun’s mass is hydrogen, and hydrogen and helium together make up about 99% of the sun’s mass. The sun’s spectrum reveals that the sun con ...
... lines of starlight to those of Earth’s elements, and identify the elements in the star’s atmosphere. Both hydrogen and helium occur in the sun. About 75% of the sun’s mass is hydrogen, and hydrogen and helium together make up about 99% of the sun’s mass. The sun’s spectrum reveals that the sun con ...
The Motions of Celestial Bodies, and Newton`s Laws of Motion
... Sir Isaac Newton and the Unification of Physics & Astronomy • Newton was by many standards the most important figure in the development of modern science. • He demonstrated that the laws that govern the heavens are the same laws that govern the motion on the surface of the Earth. • Newton's Thre ...
... Sir Isaac Newton and the Unification of Physics & Astronomy • Newton was by many standards the most important figure in the development of modern science. • He demonstrated that the laws that govern the heavens are the same laws that govern the motion on the surface of the Earth. • Newton's Thre ...
Pluto_Ceres_ASP
... (1) A planet is a celestial body that (a) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape1, and (b) is in orbit around a star, and is neither a star nor a satellite of a planet. (2) We distinguish between the ei ...
... (1) A planet is a celestial body that (a) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape1, and (b) is in orbit around a star, and is neither a star nor a satellite of a planet. (2) We distinguish between the ei ...
Problem Set 6 for Astro 320 Read sections 11.2
... Over the Sun’s main-sequence lifetime (∼ 1010 years; e.g. Fig. 13.1), the loss from nuclear fusion is 6.3 × 10−14 ∗ 1010 = 6.3 × 10−4 M . From solar wind, it’s 3 × 10−4 M . So, no substantial change. Problem 2: a) C & O, problem 11.12. The magnetic pressure in the center of a sunspot is P = B 2 /( ...
... Over the Sun’s main-sequence lifetime (∼ 1010 years; e.g. Fig. 13.1), the loss from nuclear fusion is 6.3 × 10−14 ∗ 1010 = 6.3 × 10−4 M . From solar wind, it’s 3 × 10−4 M . So, no substantial change. Problem 2: a) C & O, problem 11.12. The magnetic pressure in the center of a sunspot is P = B 2 /( ...
Elements from Stardust
... probably formed in a gigantic supernova that occurred billions of years ago. ...
... probably formed in a gigantic supernova that occurred billions of years ago. ...
Review Sheet - University of Mount Union
... 16. How did Tycho's supernova & comet contribute to the changing of ideas about the heavens? 17. Why were Galileo's observations so important? What did he observe? 18. What motion do we use to measure a day? A month? A year? 19. If you were on the Moon during a new moon, in what phase would you see ...
... 16. How did Tycho's supernova & comet contribute to the changing of ideas about the heavens? 17. Why were Galileo's observations so important? What did he observe? 18. What motion do we use to measure a day? A month? A year? 19. If you were on the Moon during a new moon, in what phase would you see ...
Formation and evolution of the Solar System
The formation of the Solar System began 4.6 billion years ago with the gravitational collapse of a small part of a giant molecular cloud. Most of the collapsing mass collected in the center, forming the Sun, while the rest flattened into a protoplanetary disk out of which the planets, moons, asteroids, and other small Solar System bodies formed.This widely accepted model, known as the nebular hypothesis, was first developed in the 18th century by Emanuel Swedenborg, Immanuel Kant, and Pierre-Simon Laplace. Its subsequent development has interwoven a variety of scientific disciplines including astronomy, physics, geology, and planetary science. Since the dawn of the space age in the 1950s and the discovery of extrasolar planets in the 1990s, the model has been both challenged and refined to account for new observations.The Solar System has evolved considerably since its initial formation. Many moons have formed from circling discs of gas and dust around their parent planets, while other moons are thought to have formed independently and later been captured by their planets. Still others, such as the Moon, may be the result of giant collisions. Collisions between bodies have occurred continually up to the present day and have been central to the evolution of the Solar System. The positions of the planets often shifted due to gravitational interactions. This planetary migration is now thought to have been responsible for much of the Solar System's early evolution.In roughly 5 billion years, the Sun will cool and expand outward many times its current diameter (becoming a red giant), before casting off its outer layers as a planetary nebula and leaving behind a stellar remnant known as a white dwarf. In the far distant future, the gravity of passing stars will gradually reduce the Sun's retinue of planets. Some planets will be destroyed, others ejected into interstellar space. Ultimately, over the course of tens of billions of years, it is likely that the Sun will be left with none of the original bodies in orbit around it.