The Sun is our local star.
... You could record information about the Sun by using a main idea and details table. ...
... You could record information about the Sun by using a main idea and details table. ...
Lesson 28 - Purdue Math
... Finally Kepler (1571-1630) is credited with discovering that the planets revolve in elliptical orbits about the sun. He wrote 3 laws of planetary motion. The first law states: The orbit of each planet in the solar system is an ellipse with the sun as one focus. (The sun is not at the center or an or ...
... Finally Kepler (1571-1630) is credited with discovering that the planets revolve in elliptical orbits about the sun. He wrote 3 laws of planetary motion. The first law states: The orbit of each planet in the solar system is an ellipse with the sun as one focus. (The sun is not at the center or an or ...
AIM: What is Astronomy? Do Now:
... **Apparent motion= what an object appears to be doing, not what it is actually doing** ...
... **Apparent motion= what an object appears to be doing, not what it is actually doing** ...
Science 9 – Space Exploration
... A. measure the angle between the Moon and any given star B. identify details in the far reaches of the night sky C. chart astronomical position and predict the movement of stars D. measure a star’s height above the horizon 8. Arabian Astronomers used an instrument, called an astrolabe to … A. measur ...
... A. measure the angle between the Moon and any given star B. identify details in the far reaches of the night sky C. chart astronomical position and predict the movement of stars D. measure a star’s height above the horizon 8. Arabian Astronomers used an instrument, called an astrolabe to … A. measur ...
Kepler`s Laws Notes
... which is near or inside the mass of the sun. If we were at that point, we could expect to see the planets move around us in planes; but, since we are on Earth and orbiting the CofM ourselves, the apparent path of a planet in our sky is complicated by combined motions on different orbits (look ahead ...
... which is near or inside the mass of the sun. If we were at that point, we could expect to see the planets move around us in planes; but, since we are on Earth and orbiting the CofM ourselves, the apparent path of a planet in our sky is complicated by combined motions on different orbits (look ahead ...
Diapozitivul 1
... • The sun is actually about 5 million kilometers closer to the earth in January than it is in July. •The average distance from the center of the sun to the center of the earth is 150 million kilometers. ...
... • The sun is actually about 5 million kilometers closer to the earth in January than it is in July. •The average distance from the center of the sun to the center of the earth is 150 million kilometers. ...
PowerPoint 2.6Mb
... so let's have "time zones" (the Sun hits the meridian at noon only in the middle of a zone) use "daylight savings time" to make it get dark later (Sun hits meridian at 1pm) (but nothing astronomical happens; this is an arbitrary convention) ...
... so let's have "time zones" (the Sun hits the meridian at noon only in the middle of a zone) use "daylight savings time" to make it get dark later (Sun hits meridian at 1pm) (but nothing astronomical happens; this is an arbitrary convention) ...
Sky Science Review for Test Part A
... S.O. 4 – Understand that the Sun should never be viewed directly, nor by the use of simple telescopes or filters, and that safe viewing requires appropriate methods and safety precautions. Looking directly at the Sun causes damage to our eyes that cannot be repaired. It is also dangerous to look ...
... S.O. 4 – Understand that the Sun should never be viewed directly, nor by the use of simple telescopes or filters, and that safe viewing requires appropriate methods and safety precautions. Looking directly at the Sun causes damage to our eyes that cannot be repaired. It is also dangerous to look ...
Intro to Space
... • You will be divided into a group of 4 or 5 • You will need to take your information from the website and design our solar system on paper • Be creative! Make sure you use the facts in some way from the website and incorporate it into your design • INCLUDE all the parts of the solar system • You wi ...
... • You will be divided into a group of 4 or 5 • You will need to take your information from the website and design our solar system on paper • Be creative! Make sure you use the facts in some way from the website and incorporate it into your design • INCLUDE all the parts of the solar system • You wi ...
ASTRO OTTER JUNIOR
... time 5:15 Topics include: the sun, the planets, terrestrial versus jovian planets, the asteroid belt, contents of the solar system, and watch the planets wander across the sky ...
... time 5:15 Topics include: the sun, the planets, terrestrial versus jovian planets, the asteroid belt, contents of the solar system, and watch the planets wander across the sky ...
15 September: Basic properties of the Sun
... The Sun has a “heartbeat”; its properties change on a period of 11 years ...
... The Sun has a “heartbeat”; its properties change on a period of 11 years ...
astronomy review sheet2
... 2. How fast and in what direction do celestial objects move across our sky? 3. Where is Polaris located and how do stars appear to move around it? 4. What is the difference between rotation and revolution? 5. Time on Earth is based on the motion of the ___________ around the _______. 6. What proof d ...
... 2. How fast and in what direction do celestial objects move across our sky? 3. Where is Polaris located and how do stars appear to move around it? 4. What is the difference between rotation and revolution? 5. Time on Earth is based on the motion of the ___________ around the _______. 6. What proof d ...
Numbers to Keep in Mind
... The Earth’s flattening and the obliquity of the ecliptic, cause the direction of the Earth’s axis to wobble on 2 timescales: § Precession causes the Earth’s axis to trace a 23.5° circle on the sky every ~26,000 years. The motion is ~ 50.3” per year east-to-west along the ecliptic (opposite the dir ...
... The Earth’s flattening and the obliquity of the ecliptic, cause the direction of the Earth’s axis to wobble on 2 timescales: § Precession causes the Earth’s axis to trace a 23.5° circle on the sky every ~26,000 years. The motion is ~ 50.3” per year east-to-west along the ecliptic (opposite the dir ...
Numbers to Keep in Mind
... Equinox and Epoch Because of the effects of precession and nutation, one must always include the equinox when quoting coordinates. These days, one usually gives right ascension and declination in J2000 coordinates (though in older papers, you’ll often see B1950 quoted). Note: many times you’ll see ...
... Equinox and Epoch Because of the effects of precession and nutation, one must always include the equinox when quoting coordinates. These days, one usually gives right ascension and declination in J2000 coordinates (though in older papers, you’ll often see B1950 quoted). Note: many times you’ll see ...
Homework 1 - Course Pages of Physics Department
... (a) Let’s assume the universe is infinite, eternal, and unchanging (and has Euclidean geometry). For simplicity, let’s also assume that all stars are the same size as the sun, and distributed evenly in space. Show that the line of sight meets the surface of a star in every direction, sooner or later ...
... (a) Let’s assume the universe is infinite, eternal, and unchanging (and has Euclidean geometry). For simplicity, let’s also assume that all stars are the same size as the sun, and distributed evenly in space. Show that the line of sight meets the surface of a star in every direction, sooner or later ...
07 September: The Solar System in a Stellar Context
... The fastest anything can travel is speed of light = c = 2.9979E+08 meters/sec Distance to Sun = 1 au = 1.496E+11 meters (see Appendix 1), so light travel time from Sun is t=d/c =1.496E+11/2.9979E+08 = t=499.02 sec A little over 8 minutes ...
... The fastest anything can travel is speed of light = c = 2.9979E+08 meters/sec Distance to Sun = 1 au = 1.496E+11 meters (see Appendix 1), so light travel time from Sun is t=d/c =1.496E+11/2.9979E+08 = t=499.02 sec A little over 8 minutes ...
The Passage of Time Moon, Moonth, Month Sidereal (Star) Time
... • 12 lunar cycles is also close to a full year; 354 days instead of 365 (12 x 29.53059 = ...
... • 12 lunar cycles is also close to a full year; 354 days instead of 365 (12 x 29.53059 = ...
Mon May 27, 2013 THE VENERABLE BEDE FEAST DAY On May
... Fri May 31, 2013 THE SUN AND THE SOLAR YEAR The sun is on the move. Now this movement I’m talking about is much more subtle than the obvious sunrise-sunset stuff we get every day, due to earth’s rotation. Assuming you could make the sun dimmer so that you could see it and stars at the same time, (so ...
... Fri May 31, 2013 THE SUN AND THE SOLAR YEAR The sun is on the move. Now this movement I’m talking about is much more subtle than the obvious sunrise-sunset stuff we get every day, due to earth’s rotation. Assuming you could make the sun dimmer so that you could see it and stars at the same time, (so ...
Space is Big…
... You just won’t believe how vastly, hugely, mindbogglingly big it is. I mean, you may think it’s a long way down the road to the chemist’s, but that’s just peanuts to space.” ...
... You just won’t believe how vastly, hugely, mindbogglingly big it is. I mean, you may think it’s a long way down the road to the chemist’s, but that’s just peanuts to space.” ...
Variable Stars: Pulsation, Evolution and applications to Cosmology
... l=m=0, pulsation purely radial. l=0,1,2,,,n-1 and m=-l+1,-l+2,….l-1 With l,m non-zero need to worry about Poisson’s equation as well. n: number of nodes radially outward from Sun’s center. m: number of nodes found around the equator. l: number of nodes found around the azimuth (great circle through ...
... l=m=0, pulsation purely radial. l=0,1,2,,,n-1 and m=-l+1,-l+2,….l-1 With l,m non-zero need to worry about Poisson’s equation as well. n: number of nodes radially outward from Sun’s center. m: number of nodes found around the equator. l: number of nodes found around the azimuth (great circle through ...
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.