Earth-Sun Relationships - Los Angeles Mission College
... A Portion of the Electromagnetic Spectrum of Radiant Energy ...
... A Portion of the Electromagnetic Spectrum of Radiant Energy ...
Chapter2
... The Motion of the Planets (3) Mercury appears at most ~28° from the sun. It can occasionally be seen shortly after sunset in the west or before sunrise in the east. Venus appears at most ~46° from the sun. ...
... The Motion of the Planets (3) Mercury appears at most ~28° from the sun. It can occasionally be seen shortly after sunset in the west or before sunrise in the east. Venus appears at most ~46° from the sun. ...
S1_LectureOutlines
... • How do we define the day, month, year, and planetary time periods? – Sidereal day (Earth’s rotation with respect to stars) is 4 minutes shorter than a solar day. – Sidereal month (27.3 day orbit of moon) is shorter then synodic month (29.5 day cycle of phases). – Tropical year (cycle of seasons) i ...
... • How do we define the day, month, year, and planetary time periods? – Sidereal day (Earth’s rotation with respect to stars) is 4 minutes shorter than a solar day. – Sidereal month (27.3 day orbit of moon) is shorter then synodic month (29.5 day cycle of phases). – Tropical year (cycle of seasons) i ...
THE PHOTOSPHERE IS THE VISIBLE SURFACE OF THE SUN
... fusion of hydrogen to helium. The core is approximately 15,000,000o C. The sun is mostly hydrogen (92% in terms of number of atoms, 75% of mass). Helium is the second most abundant element at 7.8% in terms of number of atoms and 25% in terms of mass. The sun is 0.1% other elements. The sun makes up ...
... fusion of hydrogen to helium. The core is approximately 15,000,000o C. The sun is mostly hydrogen (92% in terms of number of atoms, 75% of mass). Helium is the second most abundant element at 7.8% in terms of number of atoms and 25% in terms of mass. The sun is 0.1% other elements. The sun makes up ...
Astronomy_Main_Lesson_Book_Contents
... iv. The analemma – when a picture of the sun is taken at the same time every day Explanation of the Seasons a. Geocentric view – description of seasons and position of sun in sky and rising point, length of day b. Heliocentric view – drawing of Earth in various positions of orbit around Sun with exp ...
... iv. The analemma – when a picture of the sun is taken at the same time every day Explanation of the Seasons a. Geocentric view – description of seasons and position of sun in sky and rising point, length of day b. Heliocentric view – drawing of Earth in various positions of orbit around Sun with exp ...
Week 3
... along the horizon is fastest around the equinoxes, and slowest around the solstices Around the equinoxes, the declination (distance from the celestial equator) will change by 0.5° per day Near the solstices, it will stay fixed for almost a week ...
... along the horizon is fastest around the equinoxes, and slowest around the solstices Around the equinoxes, the declination (distance from the celestial equator) will change by 0.5° per day Near the solstices, it will stay fixed for almost a week ...
Rotation & revolution
... Summer Solstice is the longest day of the year in the Northern Hemisphere (Sun directly over Tropic of Cancer-23.5°N-at noon) Winter solstice = shortest day of the year for Northern Hemisphere (Sun directly over Tropic of ...
... Summer Solstice is the longest day of the year in the Northern Hemisphere (Sun directly over Tropic of Cancer-23.5°N-at noon) Winter solstice = shortest day of the year for Northern Hemisphere (Sun directly over Tropic of ...
Lecture 9: Hydrostatic Equilibrium
... Note that in most cases of interest in stellar structure, the radiation pressure is much less than the gas pressure and can often be neglected. The exception is the atmospheres of very hot stars, where the gas density is so low and the temperature so high that radiation pressure becomes important. A ...
... Note that in most cases of interest in stellar structure, the radiation pressure is much less than the gas pressure and can often be neglected. The exception is the atmospheres of very hot stars, where the gas density is so low and the temperature so high that radiation pressure becomes important. A ...
Solutions 1
... For the sun to appear on the zenith an observer must live between the Tropic of Cancer and the Tropic of Capricorn or between +23½ o and -23½ o of the Earth's equator (celestial equator). This is the result of the 23½ o tilt of the Earth's celestial equator with respect to the ecliptic (the path of ...
... For the sun to appear on the zenith an observer must live between the Tropic of Cancer and the Tropic of Capricorn or between +23½ o and -23½ o of the Earth's equator (celestial equator). This is the result of the 23½ o tilt of the Earth's celestial equator with respect to the ecliptic (the path of ...
Life Cycle of Our Sun
... This field attracts solar particles from the sun that could destroy all life on Earth. The field forms around the Earth’s magnetic poles, which rotate every 10,000 years. Our magnetic poles are shifting right now and will change possibly within your lifetime. The earth’s magnetic field is believ ...
... This field attracts solar particles from the sun that could destroy all life on Earth. The field forms around the Earth’s magnetic poles, which rotate every 10,000 years. Our magnetic poles are shifting right now and will change possibly within your lifetime. The earth’s magnetic field is believ ...
The Sun, Stars, and Beyond
... for “normal” convective fluid flow, which brings the heat to the surface, or photosphere. ...
... for “normal” convective fluid flow, which brings the heat to the surface, or photosphere. ...
The Motion of Celestial Bodies
... planets each move in a circle (epicycle) whose center moves on the periphery of another circle (deferent) which is in turn centered on a point slightly displaced from the Earth’s center. This geocentric world picture stood the ground for 1400 years until Nicolaus Copernicus on his death bed in 1543 ...
... planets each move in a circle (epicycle) whose center moves on the periphery of another circle (deferent) which is in turn centered on a point slightly displaced from the Earth’s center. This geocentric world picture stood the ground for 1400 years until Nicolaus Copernicus on his death bed in 1543 ...
I. Layers of the Sun
... 99% of all the matter in our solar system is in the sun. The sun is the center of the solar system. The sun is a main-sequence star. The sun produces energy by fusion. 75% Hydrogen and 25% Helium fuse in the core. ...
... 99% of all the matter in our solar system is in the sun. The sun is the center of the solar system. The sun is a main-sequence star. The sun produces energy by fusion. 75% Hydrogen and 25% Helium fuse in the core. ...
Exploring the Solar System
... Kepler’s 3rd Law of Planetary Motion • It means that if you know the period of a planet's orbit (P = how long it takes the planet to go around the Sun), then you can determine that planet's distance from the Sun (a = the semi-major axis of the planet's orbit). ...
... Kepler’s 3rd Law of Planetary Motion • It means that if you know the period of a planet's orbit (P = how long it takes the planet to go around the Sun), then you can determine that planet's distance from the Sun (a = the semi-major axis of the planet's orbit). ...
8.2 Solar Nebula Theory and the Sun
... How the Solar System Formed • Tiny grains or small lumps collect in nebula – Attract others and build up to bigger, rocky lumps called planetismals ...
... How the Solar System Formed • Tiny grains or small lumps collect in nebula – Attract others and build up to bigger, rocky lumps called planetismals ...
Astronomy 360 - indstate.edu
... • Any object ``half-way up'' in the sky is about 45 degrees above the horizon ...
... • Any object ``half-way up'' in the sky is about 45 degrees above the horizon ...
The Sun
... The inside of the Sun is made up of different layers, one inside the other. There are three layers: 1)Solar Core 2)Radiation Zone 3)Convection Zone ...
... The inside of the Sun is made up of different layers, one inside the other. There are three layers: 1)Solar Core 2)Radiation Zone 3)Convection Zone ...
Powers of ten notation
... The Sun on the other hand, takes an average of 24 hours between successive meridian crossings. The difference is due to Earth’s revolution about the Sun. The Sun moves on average 4 minutes eastward each day relative to the stars, staying in the sky longer each day than a star at the same declination ...
... The Sun on the other hand, takes an average of 24 hours between successive meridian crossings. The difference is due to Earth’s revolution about the Sun. The Sun moves on average 4 minutes eastward each day relative to the stars, staying in the sky longer each day than a star at the same declination ...
Astronomy_Main_Lesson_Book_Contents_2007
... b. Aristotle and Ptolemy – Earth-centered model c. Copernicus – Sun-centered model d. Galileo’s Discoveries: i. Phases of Venus ii. Craters on Moon iii. Sunspots iv. Moons of Jupiter v. Negative consequences for the Aristotelian/Ptolemaic model and its support for the Copernican e. Kepler’s Three La ...
... b. Aristotle and Ptolemy – Earth-centered model c. Copernicus – Sun-centered model d. Galileo’s Discoveries: i. Phases of Venus ii. Craters on Moon iii. Sunspots iv. Moons of Jupiter v. Negative consequences for the Aristotelian/Ptolemaic model and its support for the Copernican e. Kepler’s Three La ...
The Seasons (PowerPoint)
... The Earth is sometimes closer, sometimes farther away, in its orbit around the Sun. ...
... The Earth is sometimes closer, sometimes farther away, in its orbit around the Sun. ...
Unit I – The Seasons
... The Earth is sometimes closer, sometimes farther away, in its orbit around the Sun. The orientation of the Earth in its orbit matters somehow. ...
... The Earth is sometimes closer, sometimes farther away, in its orbit around the Sun. The orientation of the Earth in its orbit matters somehow. ...
The Motion of Celestial Bodies
... planets each move in a circle (epicycle) whose center moves on the periphery of another circle (deferent) which is in turn centered on a point slightly displaced from the Earth’s center. This geocentric world picture stood the ground for 1400 years until Nicolaus Copernicus on his death bed in 1543 ...
... planets each move in a circle (epicycle) whose center moves on the periphery of another circle (deferent) which is in turn centered on a point slightly displaced from the Earth’s center. This geocentric world picture stood the ground for 1400 years until Nicolaus Copernicus on his death bed in 1543 ...
Equation of time
The equation of time describes the discrepancy between two kinds of solar time. These are apparent solar time, which directly tracks the motion of the sun, and mean solar time, which tracks a fictitious ""mean"" sun with noons 24 hours apart. Apparent (or true) solar time can be obtained by measurement of the current position (hour angle) of the Sun, or indicated (with limited accuracy) by a sundial. Mean solar time, for the same place, would be the time indicated by a steady clock set so that over the year its differences from apparent solar time average to zero.The equation of time is the east or west component of the analemma, a curve representing the angular offset of the Sun from its mean position on the celestial sphere as viewed from Earth. The equation of time values for each day of the year, compiled by astronomical observatories, were widely listed in almanacs and ephemerides.