Stars: from Adolescence to Old Age
... – pressure due to fusion in core • hydrogen in the core eventually converted to helium nuclear reactions stop! • gravity takes over and the core shrinks • outside layers also collapse • layers closer to the center collapse faster than those near the surface. • As the layers collapses, the gas comp ...
... – pressure due to fusion in core • hydrogen in the core eventually converted to helium nuclear reactions stop! • gravity takes over and the core shrinks • outside layers also collapse • layers closer to the center collapse faster than those near the surface. • As the layers collapses, the gas comp ...
1. What are the four branches of earth? -Geology
... When the sun is at its highest point in the sky it is 12pm noon. Because of the suns movements from east to west the sun will appear at different locations throughout the day and that will be that locations 12 pm noon because of its highest location in the sky at that location. This allows for diffe ...
... When the sun is at its highest point in the sky it is 12pm noon. Because of the suns movements from east to west the sun will appear at different locations throughout the day and that will be that locations 12 pm noon because of its highest location in the sky at that location. This allows for diffe ...
Foundation 1 - Discovering Astronomy
... graduate student Jocelyn Bell. • She found a radio source with a regular on-off-on cycle of exactly 1.3373011 seconds. • Some scientists speculated that this was evidence of an alien civilization’s communication system and dubbed the source LGM (Little Green Men!!!) • Today, we know pulsars are rapi ...
... graduate student Jocelyn Bell. • She found a radio source with a regular on-off-on cycle of exactly 1.3373011 seconds. • Some scientists speculated that this was evidence of an alien civilization’s communication system and dubbed the source LGM (Little Green Men!!!) • Today, we know pulsars are rapi ...
Gravitational Forces
... (c) (i) Calculate the gravitational field strength at the surface of a planet that has the same density as the Earth but with a radius that is 3.5 times less than the Earth’s . ___________________________________________________________________________________ _______________________________________ ...
... (c) (i) Calculate the gravitational field strength at the surface of a planet that has the same density as the Earth but with a radius that is 3.5 times less than the Earth’s . ___________________________________________________________________________________ _______________________________________ ...
The Jerusalem Teddy Park Sundial
... time zone. The standard time at any place is coordinated by fixed time zones, and does not take into account the specifics of the local coordinates where the sundial is situated. Every 15 degrees in longitude are equal to one hour in time, or one degree corresponds to 4 minutes in time. This means t ...
... time zone. The standard time at any place is coordinated by fixed time zones, and does not take into account the specifics of the local coordinates where the sundial is situated. Every 15 degrees in longitude are equal to one hour in time, or one degree corresponds to 4 minutes in time. This means t ...
Black Hole
... Stars born with more then 8 — 10 M cannot lose enough mass to become white dwarfs. These stars die by exploding as Supernovae II. Ignition of “metals” During periods when the core of a star is not hot enough so that its nuclei can produce energy by fusion, it nevertheless must be extremely hot to h ...
... Stars born with more then 8 — 10 M cannot lose enough mass to become white dwarfs. These stars die by exploding as Supernovae II. Ignition of “metals” During periods when the core of a star is not hot enough so that its nuclei can produce energy by fusion, it nevertheless must be extremely hot to h ...
Here
... wavelengths? 13. What is a blackbody? What does it mean to say that a star appears almost like a black body? … 15. What is Wien’s Law? How could you use it to determine the temperature of a star’s surface? 16. What is the Stefan-Boltzmann law? How do Astronomers us it? ...
... wavelengths? 13. What is a blackbody? What does it mean to say that a star appears almost like a black body? … 15. What is Wien’s Law? How could you use it to determine the temperature of a star’s surface? 16. What is the Stefan-Boltzmann law? How do Astronomers us it? ...
1705 Star Charts
... Saucepan, now lying on its side. In early June Orion can be seen both in the west at dusk and in the east at dawn. The Orion Nebula is visible in binoculars as a misty glow around the middle star of Orion's Sword or the handle of The Pot. It is a vast cloud of dust and gas about 1300 l.y. away and m ...
... Saucepan, now lying on its side. In early June Orion can be seen both in the west at dusk and in the east at dawn. The Orion Nebula is visible in binoculars as a misty glow around the middle star of Orion's Sword or the handle of The Pot. It is a vast cloud of dust and gas about 1300 l.y. away and m ...
Unit 6: Astronomy
... Copernicus lived during the height of the Renaissance period when men from a higher social class were expected to receive well-rounded educations. In 1491, Copernicus attended the University of Krakow where he studied mathematics and astronomy. After four years of study, his uncle appointed Copernic ...
... Copernicus lived during the height of the Renaissance period when men from a higher social class were expected to receive well-rounded educations. In 1491, Copernicus attended the University of Krakow where he studied mathematics and astronomy. After four years of study, his uncle appointed Copernic ...
Chapter-by-Chapter Guide
... looking farther away means looking further back in time. The observable universe is the portion of the entire universe that we can, in principle, see. It is presumably about 14 billion light-years in radius because light from more than 14 billion light-years away could not yet have reached us during ...
... looking farther away means looking further back in time. The observable universe is the portion of the entire universe that we can, in principle, see. It is presumably about 14 billion light-years in radius because light from more than 14 billion light-years away could not yet have reached us during ...
Chapter 2: The Solar System and Beyond
... Compare and contrast spring tides and neap tides. Think Critically What would seasons be like if Earth’s axis were tilted at a higher angle (more than 23.5°)? ...
... Compare and contrast spring tides and neap tides. Think Critically What would seasons be like if Earth’s axis were tilted at a higher angle (more than 23.5°)? ...
The Rise of Solar Cycle 24
... magnetograms (factors of up to 4). We don’t know actual value of magnetic fields at photosphere. Alex Pestov: ...
... magnetograms (factors of up to 4). We don’t know actual value of magnetic fields at photosphere. Alex Pestov: ...
Oct 2011 - Bays Mountain Park
... planet has many different features to observe and is especially nice if the sky is steady. The first thing to catch your attention are the two dark equatorial belts on either side of the equator. One of these belts was absent for most of last year and we have no idea why it should act that way. Any g ...
... planet has many different features to observe and is especially nice if the sky is steady. The first thing to catch your attention are the two dark equatorial belts on either side of the equator. One of these belts was absent for most of last year and we have no idea why it should act that way. Any g ...
Star Fromation and ISM
... • The protostar continues to collapse; when the core is dense and hot enough, fusion begins • The star still continues to collapse until the inward force of gravity is balanced by the outward pressure from the core. The star is now on the main sequence. • More massive stars follow the same process, ...
... • The protostar continues to collapse; when the core is dense and hot enough, fusion begins • The star still continues to collapse until the inward force of gravity is balanced by the outward pressure from the core. The star is now on the main sequence. • More massive stars follow the same process, ...
The celestial sphere, the coordinates system, seasons, phases of
... total of 7,000 km. An observer located inside this strip will see a total solar eclipse. Partial solar eclipse: If the observer is located in the penumbral part of the shadow, only part of the Sun will be covered and the observer will see a partial solar eclipse Annular solar eclipse: If the Moon is ...
... total of 7,000 km. An observer located inside this strip will see a total solar eclipse. Partial solar eclipse: If the observer is located in the penumbral part of the shadow, only part of the Sun will be covered and the observer will see a partial solar eclipse Annular solar eclipse: If the Moon is ...
Lecture 10: The Milky Way
... This gives us the absolute luminosities of low-mass stars, and using binary systems we can calibrate our models to true masses and radii (see earlier). The trouble is that within 100pc we have no massive stars and only 4 giants – how do we calibrate these? To get distances to objects further away we ...
... This gives us the absolute luminosities of low-mass stars, and using binary systems we can calibrate our models to true masses and radii (see earlier). The trouble is that within 100pc we have no massive stars and only 4 giants – how do we calibrate these? To get distances to objects further away we ...
Stellar Evolution Before…..During……and After…. The Main
... • The length of time a star spends fusing hydrogen into helium is called its main sequence lifetime ...
... • The length of time a star spends fusing hydrogen into helium is called its main sequence lifetime ...
The Milky Way Galaxy
... To determine the rotation curve of the Galaxy, we will introduce a more convenient coordinate system, called the Galactic coordinate system. Note that the plane of the solar system is not the same as the plane of the Milky Way disk, and the Earth itself is tipped with respect to the plane of the sol ...
... To determine the rotation curve of the Galaxy, we will introduce a more convenient coordinate system, called the Galactic coordinate system. Note that the plane of the solar system is not the same as the plane of the Milky Way disk, and the Earth itself is tipped with respect to the plane of the sol ...
Notes (PowerPoint)
... • Star – source of light (gravity has crushed atoms to start nuclear reactions) • Planet – large, opaque, nonluminous, circles a star (Pluto is on the smallish side) • Moon – a natural satellite of a planet • Asteroid – Small planet, size from 1 km (.6 mi) to ...
... • Star – source of light (gravity has crushed atoms to start nuclear reactions) • Planet – large, opaque, nonluminous, circles a star (Pluto is on the smallish side) • Moon – a natural satellite of a planet • Asteroid – Small planet, size from 1 km (.6 mi) to ...
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.