Word version
... days—to complete. Careful observers learned to count out these days and created the first calendars. Solar and lunar cycles don’t line up precisely, however: the 29 and a half days of a lunar month do not fit evenly into the 365 days of the solar year. A calendar based on the moon will shift by abou ...
... days—to complete. Careful observers learned to count out these days and created the first calendars. Solar and lunar cycles don’t line up precisely, however: the 29 and a half days of a lunar month do not fit evenly into the 365 days of the solar year. A calendar based on the moon will shift by abou ...
A Compilation of Relevant Articles from MMM`s first 25 years, issues
... We've all seen the phrase "Earthlike Worlds" but just what does it mean? Different things to different people, of course. And that's because it is intrinsically imprecise, since there are so many varying definitions of just what the "essence of Earth" is. Some people use the term in contradistinctio ...
... We've all seen the phrase "Earthlike Worlds" but just what does it mean? Different things to different people, of course. And that's because it is intrinsically imprecise, since there are so many varying definitions of just what the "essence of Earth" is. Some people use the term in contradistinctio ...
Why do Earth satellites stay up?
... “there are only periodic oscillations in the perigee and these are too small to be important” or “the orbits are unstable but on timescales much longer than the satellite lifetime”. We shall show that neither of these answers captures the most relevant physics. The primary goal of this paper is to u ...
... “there are only periodic oscillations in the perigee and these are too small to be important” or “the orbits are unstable but on timescales much longer than the satellite lifetime”. We shall show that neither of these answers captures the most relevant physics. The primary goal of this paper is to u ...
Analytic Models for the Mechanical Structure of the Solar Core
... In the homogeneous ZAMS Sun, 1 + ne ≡ d ln P/d ln(P/ρ) is identical to 1 + N ≡ d ln P/d ln T ≡ 1/∇ and varies from the almost adiabatic value 2.52 at z = 0 to a maximum value 5.21 at z = 0.32 (r = 0.506 of ZAMS solar radius). Where the radiative zone meets the convective core, 1 + ne shows a discont ...
... In the homogeneous ZAMS Sun, 1 + ne ≡ d ln P/d ln(P/ρ) is identical to 1 + N ≡ d ln P/d ln T ≡ 1/∇ and varies from the almost adiabatic value 2.52 at z = 0 to a maximum value 5.21 at z = 0.32 (r = 0.506 of ZAMS solar radius). Where the radiative zone meets the convective core, 1 + ne shows a discont ...
September 2016
... overhead is known as the Zenith or Nadir and is shown at the upper centre of the chart. The curved brown line across the sky at the bottom is the Ecliptic or Zodiac. This is the imaginary line along which the Sun, Moon and planets appear to move across the sky. The constellations through which the e ...
... overhead is known as the Zenith or Nadir and is shown at the upper centre of the chart. The curved brown line across the sky at the bottom is the Ecliptic or Zodiac. This is the imaginary line along which the Sun, Moon and planets appear to move across the sky. The constellations through which the e ...
Slides for Earth and the Solar System Unit #1
... Ceres resides in the main asteroid belt between Mars and Jupiter. It was discovered in 1801 and was labeled as a planet. It kept this title for nearly half a century before being deemed a large asteroid, and now a dwarf planet. (We will figure out the difference between an asteroid and a dwarf plane ...
... Ceres resides in the main asteroid belt between Mars and Jupiter. It was discovered in 1801 and was labeled as a planet. It kept this title for nearly half a century before being deemed a large asteroid, and now a dwarf planet. (We will figure out the difference between an asteroid and a dwarf plane ...
Variability of solar/stellar activity and magnetic field and its influence... planetary atmosphere evolution
... to study the consequences this might have had for the development of the planetary environments, including the formation and evolution of planetary atmospheres and initial H2 O inventories. To understand the impacts of the radiation and particle environment of the young Sun or other stars on early p ...
... to study the consequences this might have had for the development of the planetary environments, including the formation and evolution of planetary atmospheres and initial H2 O inventories. To understand the impacts of the radiation and particle environment of the young Sun or other stars on early p ...
PP Chapter 27 Text
... • No definite surface as occurs on the inner rocky planets • Solid core of iron, nickel, and other minerals Because of its thick atmospheric blanket, daytime and nighttime temperatures are about the same for equal altitudes above its “surface.” ...
... • No definite surface as occurs on the inner rocky planets • Solid core of iron, nickel, and other minerals Because of its thick atmospheric blanket, daytime and nighttime temperatures are about the same for equal altitudes above its “surface.” ...
The production and updating of experimental results
... Galileo and the moons of Jupiter Late in 1609, Galileo constructed a powerful telescope and used it to look at the heavens. Many of the novel observations he made in the ensuing three months were controversial, and very relevant to the astronomical debate concerning the validity of the Copernican th ...
... Galileo and the moons of Jupiter Late in 1609, Galileo constructed a powerful telescope and used it to look at the heavens. Many of the novel observations he made in the ensuing three months were controversial, and very relevant to the astronomical debate concerning the validity of the Copernican th ...
Where to Look For Life? - Journey through the Universe
... There are not many other places in the Solar System where liquid water might exist. Most other places in the Solar System seem either too hot (e.g., Mercury, Venus) or likely too cold (e.g., the outer planets and their moons) for liquid water. On Mars, the surface temperature and air pressure are bo ...
... There are not many other places in the Solar System where liquid water might exist. Most other places in the Solar System seem either too hot (e.g., Mercury, Venus) or likely too cold (e.g., the outer planets and their moons) for liquid water. On Mars, the surface temperature and air pressure are bo ...
Scientific requirements of ALMA, and its capabilities for key
... Image gas kinematics in protostars and protoplanetary disks around Sun-like stars at 140pc distance, enabling one to study their physical, chemical and magnetic field structures and to detect the gaps created by planets undergoing formation in the disk. Provide precise images at 0.1 arcsec resolutio ...
... Image gas kinematics in protostars and protoplanetary disks around Sun-like stars at 140pc distance, enabling one to study their physical, chemical and magnetic field structures and to detect the gaps created by planets undergoing formation in the disk. Provide precise images at 0.1 arcsec resolutio ...
Asteroids
... Asteroids are very small, rocky bodies that orbit the Sun. "Asteroid" means "star-like," and in a telescope, asteroids look like points of light, just like stars. Asteroids are irregularly shaped because they do not have enough gravity to become round. They are also too small to maintain an atmosphe ...
... Asteroids are very small, rocky bodies that orbit the Sun. "Asteroid" means "star-like," and in a telescope, asteroids look like points of light, just like stars. Asteroids are irregularly shaped because they do not have enough gravity to become round. They are also too small to maintain an atmosphe ...
3. Meteorites and Asteroids
... grains in these meteorites are composed of hydrated silicate minerals and may contain up to 20 percent water. They are also rich in other volatile elements, but they also have flecks of metallic iron and other inclusions that formed at very high temperatures. Carbonaceous meteorites have low densiti ...
... grains in these meteorites are composed of hydrated silicate minerals and may contain up to 20 percent water. They are also rich in other volatile elements, but they also have flecks of metallic iron and other inclusions that formed at very high temperatures. Carbonaceous meteorites have low densiti ...
W. M. White Geochemistry Chapter 10: Cosmochemistry
... we learn about the evolution of the Earth by examining old rocks, we can learn about the evolution of the cosmos by looking at old stars. The old stars of Population II are considerably poorer in heavy elements than are young stars. In particular, Population II stars have a Fe/H ratio typically a fa ...
... we learn about the evolution of the Earth by examining old rocks, we can learn about the evolution of the cosmos by looking at old stars. The old stars of Population II are considerably poorer in heavy elements than are young stars. In particular, Population II stars have a Fe/H ratio typically a fa ...
Lesson 3: The Motion of the Moon, Sun, and Stars— Motivating
... motion of the sun and the planets. If just the system of Earth and the sun are considered, disregarding the other planets, then Earth and the sun both revolve around the center of mass of the system, called the barycenter. Because the mass of the sun, 1.99 × 1030 kg, is far greater than the mass of ...
... motion of the sun and the planets. If just the system of Earth and the sun are considered, disregarding the other planets, then Earth and the sun both revolve around the center of mass of the system, called the barycenter. Because the mass of the sun, 1.99 × 1030 kg, is far greater than the mass of ...
Lesson 1 | Earth`s Motion
... 2. Explain the two major motions of Earth in space that can be observed and justified by the geocentric model. ...
... 2. Explain the two major motions of Earth in space that can be observed and justified by the geocentric model. ...
PDF format
... a) There won't be enough time for a star to form before gas is blown away by neighboring stars. b) Gravity will be too weak to make the cloud collapse into a star. c) It will never get hot enough for fusion to start. d) The cloud will form planets instead of a star. © 2014 Pearson Education, Inc ...
... a) There won't be enough time for a star to form before gas is blown away by neighboring stars. b) Gravity will be too weak to make the cloud collapse into a star. c) It will never get hot enough for fusion to start. d) The cloud will form planets instead of a star. © 2014 Pearson Education, Inc ...
The Habitability of Our Earth and Other Earths: Astrophysical
... Chlorophyll maps of the ocean (McClain et al. 2006) show regions where, despite ample water, photons, and nitrates, there are low concentrations of chlorophyll. Iron fertilization experiments in these enigmatic high-nitrate-low-chlorophyll regions found that the biomass was iron limited, rather than ...
... Chlorophyll maps of the ocean (McClain et al. 2006) show regions where, despite ample water, photons, and nitrates, there are low concentrations of chlorophyll. Iron fertilization experiments in these enigmatic high-nitrate-low-chlorophyll regions found that the biomass was iron limited, rather than ...
Ch 28-31 Lessons
... 5. Of the orbits that you drew, which loop size and what color created the most eccentric (oval) ellipse? (Hint – the one with the biggest # in Column 5.) _______________________________________________________________ 6. Look at Appendix J on p. 921. There is a row labeled Orbital eccentricity. Loo ...
... 5. Of the orbits that you drew, which loop size and what color created the most eccentric (oval) ellipse? (Hint – the one with the biggest # in Column 5.) _______________________________________________________________ 6. Look at Appendix J on p. 921. There is a row labeled Orbital eccentricity. Loo ...
UCLA 2004
... When 1 Ori C goes supernova, all the disks in the Orion Nebula will be pelted with radioactive ejecta Even more true for the disks observed in Carina Nebula, with sixty O stars [Smith et al. (2003)], many other H II regions Ejecta dust grains penetrate disk, evaporate on entry, but leave SLRs lodg ...
... When 1 Ori C goes supernova, all the disks in the Orion Nebula will be pelted with radioactive ejecta Even more true for the disks observed in Carina Nebula, with sixty O stars [Smith et al. (2003)], many other H II regions Ejecta dust grains penetrate disk, evaporate on entry, but leave SLRs lodg ...
Planetesimal collisions in binary systems
... We consider the problem of planetesimal evolution in tight binary star systems such as γ Cephei and α Centauri. To date several hundred extrasolar planets have been detected – 20% of which orbit the primary of a binary or multiple system (Desidera & Barbieri 2007). In most of these cases the stars a ...
... We consider the problem of planetesimal evolution in tight binary star systems such as γ Cephei and α Centauri. To date several hundred extrasolar planets have been detected – 20% of which orbit the primary of a binary or multiple system (Desidera & Barbieri 2007). In most of these cases the stars a ...
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.