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LUNAR ECLIPSES Credit: Johannes Schedler TABLE OF CONTENTS: SAFETY ANATOMY OF A LUNAR ECLIPSE PENUMBRAL ECLIPSES PARTIAL ECLIPSES TOTAL ECLIPSES REVIEW ECLIPSE TYPES DANJON SCALE NEXT ECLIPSES Click logo anytime MORE to come back here: Credit: Johannes Schedler SAFETY Lunar eclipses are perfectly safe to view without protection. You can use your eyes, binoculars or telescopes. Be patient, it takes time for the lunar disc to change color. Credit: Johannes Schedler Credit: starrynight.com ANATOMY OF AN ECLIPSE Umbra Penumbra Frontal view of Earth’s shadow. A lunar eclipse happens when Earth comes between the Sun and the Moon, projecting its shadow onto our satellite. Shadows come in 2 forms: the penumbra which is the outmost and is partly- shaded; and the umbra, which is the innermost and is fully-shaded. PENUMBRAL ECLIPSE Umbra Penumbra Penumbral eclipses can be total, when the whole Moon enters the penumbra; or partial, when a fraction of the Moon enters the penumbra. They are difficult to detect because the Moon only changes its brightness a bit. Example of a partial penumbral eclipse. Credit: Hong Kong Space Museum PARTIAL ECLIPSE Umbra Penumbra Partial umbral eclipses take place when a fraction of the Moon enters the umbra, and of course, in its way it also enters the penumbra. When in the umbra, the lunar disc will change color or become very dark. Example of a partial umbral eclipse. Credit: Rodney Pommier TOTAL ECLIPSE Umbra Penumbra Total umbral eclipses take place when all of the Moon enters the umbra, and of course, in its way also the penumbra. When in the umbra, the lunar disc will change color or become very dark. Example of a total umbral eclipse. REVIEW ECLIPSE TYPES Credit: Tom Ruen / Wikipedia Review of lunar eclipse types DANJON SCALE 1 2 3 4 5 During the maximum of a total umbral eclipse we can see what color the lunar disc has taken and assign a value according to the Danjon Scale. Credit: Tim Trott DANJON SCALE 0 very dark totality, with the Moon almost invisible 1 dark/gray/brownish, details distinguishable with difficulty 2 deep red/rust, very dark central shadow, bright outer edge 3 brick-red with a bright or yellow rim 4 bright copper-red/orange, with a bluish & very bright rim NEXT ECLIPSES Visible in the continental USA Date Type March 23, 2016 penumbral February 11, 2017 penumbral January 31, 2018 total MORE Our website: www.astro.ucr.edu Facebook: facebook.com/astroucr Twitter: @astroucr.

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Lunar Eclipse? a Lunar Eclipse
What Causes a Lunar Eclipse? A Lunar Eclipse An eclipse of the Moon (lunar eclipse) occurs when a full moon moves into the shadow of the Earth. The Earth blocks some of the sunlight that would otherwise shine on the face of the Moon. From our position on Earth it looks as though a dark Earth’s Orbital plane Sun Earth Moon spot is moving across the Moon. The Moon travels once around the Earth every month. Why don’t we see an eclipse every month? The Earth orbits in a plane called the ecliptic. The Moon’s orbit is tilted slightly at 5 degrees. This means that there are only two points where the Moon crosses the ecliptic plane. These spots, called nodes, are the only places where the Moon will line up with the Earth and the Sun. The rest of its orbit is either above or below the Earth’s orbital plane. Descending Node Moon’s Orbital Path The Ecliptic (Earth’s Orbital Plane) 5° Ascending Node Lunar Eclipse An eclipse only occurs when the Moon, the Earth and the Sun all line up in the same plane. If the Earth is between the Sun and the Moon and the Moon is full when it crosses a node, a lunar eclipse can occur. The Earth will cast a shadow on the Moon. Solar Eclipse However, another type of eclipse will occur if the Moon lines up with a node between the Sun and the Earth. A solar eclipse will take place in this event. The Moon blocks the Earth’s view of the light of the Sun.
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Solar and Lunar Eclipses Reading
Eclipses What would you think if you were walking home from school on a sunny afternoon and the sun began to disappear? Would you be frightened? On rare occasions, the moon completely blocks the sun. The sky grows as dark as night even in the middle of a clear day. The air gets cool and the sky becomes an eerie color. If you don’t know what is happening, you can become very frightened. The moon doesn’t usually go directly between Earth and the sun or directly behind Earth. As the diagram below shows, the moon’s orbit around Earth is slightly tilted with respect to Earth’s orbit around the sun. As a result, in most months the moon revolves completely around Earth without the moon moving into Earth’s shadow or the moon’s shadow hitting Earth. When the moon’s shadow hits Earth or Earth’s shadow hits the moon, an eclipse occurs. An eclipse (ih klips) occurs when an object in space comes between the sun and a third object, and casts a shadow on that object. There are two types of eclipses: solar eclipses and lunar eclipses. (The words solar and lunar come from the Latin words for “sun” and “moon.”) The Tilt of the Moon’s Orbit The moon’s orbit is tilted with respect to Earth’s orbit. So the moon rarely goes directly between Earth and the sun. Solar Eclipses During a new moon, the moon is almost exactly between Earth and the sun. But most months, as you have seen, the moon travels a little above or below the sun in the sky.
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The Moon and Eclipses
Lecture 10 The Moon and Eclipses Jiong Qiu, MSU Physics Department Guiding Questions 1. Why does the Moon keep the same face to us? 2. Is the Moon completely covered with craters? What is the difference between highlands and maria? 3. Does the Moon’s interior have a similar structure to the interior of the Earth? 4. Why does the Moon go through phases? At a given phase, when does the Moon rise or set with respect to the Sun? 5. What is the difference between a lunar eclipse and a solar eclipse? During what phases do they occur? 6. How often do lunar eclipses happen? When one is taking place, where do you have to be to see it? 7. How often do solar eclipses happen? Why are they visible only from certain special locations on Earth? 10.1 Introduction The moon looks 14% bigger at perigee than at apogee. The Moon wobbles. 59% of its surface can be seen from the Earth. The Moon can not hold the atmosphere The Moon does NOT have an atmosphere and the Moon does NOT have liquid water. Q: what factors determine the presence of an atmosphere? The Moon probably formed from debris cast into space when a huge planetesimal struck the proto-Earth. 10.2 Exploration of the Moon Unmanned exploration: 1950, Lunas 1-3 -- 1960s, Ranger -- 1966-67, Lunar Orbiters -- 1966-68, Surveyors (first soft landing) -- 1966-76, Lunas 9-24 (soft landing) -- 1989-93, Galileo -- 1994, Clementine -- 1998, Lunar Prospector Achievement: high-resolution lunar surface images; surface composition; evidence of ice patches around the south pole.
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Low Energy Secondary Cosmic Ray Flux (Gamma Rays) Monitoring and Its Constrains
Low energy secondary cosmic ray flux (gamma rays) monitoring and its constrains Anil Raghav1,∗, Ankush Bhaskar1, Virendra Yadav1, Nitinkumar Bijewar1 1. Department of Physics, University of Mumbai,Vidyanagari, Santacruz (E), Mumbai-400098, India. 2. Indian Institute of Geomagnetism, Kalamboli Highway, New Panvel, Navi Mumbai- 410218, India. Abstract Temporal variation of secondary cosmic rays (SCR) flux was measured during the several full and new moon and days close to them at Department of Physics, University of Mumbai, Mumbai (Geomagnetic latitude: 10.6◦ N), India. The measurements were done by using NaI (Tl) scintillation detector with energy threshold of 200 keV. The SCR flux shows sudden enhance- ment for approximately about 2 hour in counts during couple of events out of all experimental observations. The maximum Enhancement SCR flux is about 200% as compared to the diurnal trend of SCR temporal variations. Weather parameters (temperature and relative humidity) were continuously monitored during all observation. The influences of geomagnetic field, in- terplanetary parameters and tidal effect on SCR flux have been considered. Summed spectra corresponding to enhancement duration indicates appear- ance of atmospheric radioactivity which shows single gamma ray line. Detail investigation revealed the presence of radioactive Ar41. This measurements puts limitations on low energy SCR flux monitoring. This paper will help arXiv:1408.1761v1 [astro-ph.EP] 8 Aug 2014 many researcher who want to measure SCR flux during eclipses and motivate to find unknown mechanism behind decrease/ increase during solar/lunar eclipse. Keywords: Secondary Cosmic Ray (SCR), terrestrial gamma ray emission, ✩ ∗corresponding author Email address: [email protected] (Anil Raghav) Preprint submitted to Arxiv August 11, 2014 Atmospheric radioactivity, lunar tides, geomagnetic field, thermal neutron burst, newmoon, fullmoon 1.
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Solstices & Equinoxes –Precession – Phases of the Moon –Eclipses
Today –Solstices & Equinoxes –Precession –Phases of the Moon –Eclipses • Lunar, Solar –Ancient Astronomy FIRST HOMEWORK DUE NEXT TIME © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Tropic: Latitude where the sun [just] reaches the zenith at noon on the summer solstice Arctic/Antarctic Circle: Latitude where the sun does not set [just barely] on the summer solstice (like a circumpolar star) nor does it rise on the winter solstice o N 66.5 arctic Ecliptic plane Tropic of Cancer 23.5o Tropic of Capricorn Equator antarctic © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Seasonal changes are more extreme at high latitudes. Path of the Sun on the summer solstice at the Arctic Circle © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley How does the orientation of Earth’s axis change with time? Precession: • Although the axis seems fixed on human time scales, it actually precesses over about 26,000 years. — Polaris won’t always be the North Star. Earth’s axis wobbles like the axis of a spinning top. © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley • Precession: the orientation of Earth’s axis slowly changes with time: — The tilt remains about 23.5 degrees (so the season pattern is not affected), but Earth has a 26,000 year precession cycle that slowly and subtly changes the orientation of the Earth’s axis. — The discovery of precession is attributed to the Ancient Greek astronomer Hipparchus (c. 280 BC) © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Lunar phases • Lunar phases are a consequence of the Moon’s 27.3-day orbit around Earth.
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Eclipse Prediction and the Length of the Saros in Babylonian Astronomy
Eclipse Prediction and the Length of the Saros in Babylonian Astronomy ∗ LIS BRACK-BERNSEN AND JOHN M. STEELE† Abstract. The Saros cycle of 223 synodic months played an important role in Late Babylonian astronomy. It was used to predict the dates of future eclipse possibilities together with the times of those eclipses and underpinned the development of mathematical lunar theories. The excess length of the Saros over a whole number of days varies due to solar and lunar anomaly between about 6 and 9 h. We here investigate two functions which model the length of the Saros found in Babylonian sources: a simple zigzag function with an 18-year period presented on the tablet BM 45861 and a function which varies with the month of the year constructed from rules found on the important procedure text TU 11. These functions are shown to model nature very well and to be closely related. We further conclude that these functions are the likely source of the Saros lengths used to calculate the times of predicted eclipses and were probably known by at latest the mid-sixth-century BC. 1. Eclipse Prediction and the Saros Throughout most, perhaps all, of the Late Babylonian period, the basic method of predict- ing eclipses of the sun and moon in Babylonia was based upon the so-called Saros cycle (SC) of 223 synodic months. This method was not restricted to simply identifying dates 1 or more Saroi after a visible eclipse but could be used to identify the dates of all eclipse possibilities (EPs). It almost certainly originated with lunar eclipses and was then applied to solar eclipses.
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W:09/19/18 Eclipses
PHYS 1411 Intro to Astronomy Extra Credit Homework Announcement Assigned on MindTap for Chapter 1, 2, 3 Due Monday December 3rd , 2018 @ 5:00 am Topics for Today’s Class Topics for Today’s Class • Chapter 3: Lunar Eclipse • Chapter 3: Solar eclipse – How to make a shadow or an eclipse? – What is a Solar eclipse? – Types of shadows – How to safely observe Solar eclipse – The importance of angular diameter in – Types of Solar eclipse eclipses – Some examples and dates – What is a Lunar eclipse? – Conditions for Solar and Lunar eclipses to – Types of Lunar eclipses occur – Why Pinkish Moon during Lunar eclipse? – Saros Cycle The Angular Diameters of the How to make a shadow? Sun & Moon • The shadow cast by a map tack can be used to understand how shadows produce eclipses – Umbra = The region of total shadow – Penumbra = The region of partial shadow – Penumbra = The region of partial shadow 1 Angular Size and Distance Two Types of Movements Increasing Distance from Eye Dime Quarter Partial Total Annular Not Visible Transit Occultation View from Eye View from Eye What is a Lunar Eclipse? Small Angle Formula Earth’s shadow consists of a zone of partial angular diameter linear diameter shadow, the Penumbra, 206,265 distance and a zone of full shadow, Example for Moon the Umbra. angular diameter 3476 km 206,26 5 384,000 km 1870 angular diameter 187 0 0.5 60 60 If the moon passes through Earth’s full shadow (Umbra), we see a lunar eclipse. If the entire surface of the moon enters Angular Diameter of Sun and Moon is important for Eclipses to occur the Umbra, the lunar eclipse is total.
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Danjon-Scale Ratings
Danjon Scale of Lunar Eclipse Brightness Around 1920, the French astronomer André-Louis Danjon devised a 5-point scale (0 to 4) for cataloguing the Luminosity “L” and color of lunar eclipses. Here is the scale: L = 0 Very dark moon, almost invisible. L = 1 Dark gray or brownish moon; details on moon not visible. L = 2 Deep red or rust-colored moon; can see some details. L = 3 Brick-red colored moon; details on moon are visible. L = 4 Bright copper-red or orange colored moon; details easy to see. Eclipse Quiz: Now, hone your skill at estimating the “L” values of seven different eclipses. Each “test” slide is followed by the same slide with the best estimate highlighted. If you can’t decide between two L values, say 2 and 3, you may split the difference and call it 2.5, for example. When making estimates of a real eclipse, be sure to use your unaided eye (glasses or contact lenses are OK), and NOT binoculars or telescope. And note the time! A. L = 0 Very dark moon, almost invisible. B. L = 1 Dark gray or brownish moon; details on moon not visible. C. L = 2 Deep red or rust-colored moon; can see some details. D. L = 3 Brick-red colored moon; details on moon are visible. E. L = 4 Bright copper-red or orange colored moon; details easy to see. A. L = 0 Very dark moon, almost invisible. B. L = 1 Dark gray or brownish moon; details on moon not visible. C. L = 2 Deep red or rust-colored moon; can see some details.
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Lunar Phases & Eclipses
Today FIRST HOMEWORK DUE NEXT TIME Seasons/Precession Recap Phases of the Moon Eclipses Lunar, Solar Ancient Astronomy 1 Extra credit (2 points) • What is the main cause of seasons on Earth? • Be sure to include your name and section number • You may consult your notes, but do not communicate with anyone else 2 © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Reminder: HW due Thursday • Must turn in before 9:30 AM Thursday • E-mail, in PDF form, to: [email protected] (e.g., astro100-0103 if you are in section 0103) • Must be typed, not scanned PDF If you need help converting from Word or other programs, talk with your TA • Good luck! 3 © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Summary of seasons and precession • Marking the progression of the seasons: —Our summer and winter solstices are when the Northern Hemisphere gets its most and least direct sunlight, respectively. The spring and fall equinoxes are when both hemispheres get equally direct sunlight. • Precession: the orientation of Earth’s axis slowly changes with time: —The tilt remains about 23.5 degrees (so the season pattern is not affected), but Earth has a 26,000 year precession cycle that slowly and subtly changes the orientation of the Earth’s axis. —The discovery of precession is attributed to the Ancient Greek astronomer Hipparchus (c. 280 BC) 4 © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Apparent Location of Sun From College Park, when does the Sun appear to be directly overhead (i.e., at the zenith)? A.Noon on the equinoxes B.
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Lunar Phases
Observing the Moon Moon (Luna): - changes position in sky - goes around Cel. Sphere in ~1 month - changes appearance: “Phase” - depends on locations of Earth, Moon and Sun Moon revolves around the Earth: Same direction as Earth rotates - Follows “Right-Hand Rule” We can only see portion of the Moon that is illuminated by sunlight New Moon: (beginning of lunar month) - moon is between earth & sun - sunlit side faces away from earth What we see: - Moon is not visible (0% illuminated as seen from Earth) Sun-lit portion of moon gets larger (as seen from earth) - "Waxing" What we see: Waxing Crescent Crescent = less than half full (<50% illuminated) What we see: First Quarter (50% Illuminated) What we see: Waxing Gibbous Gibbous = more than half full (> 50% illuminted) Full Moon: - on opposite side (180o) from sun - entire sunlit side facing earth What we see: (100% Illuminated) Sun-lit portion decreases - waning What we see: http://stardate.org/nightsky/moon/ http://www.astro.wisc.edu/~dolan/java/MoonPhase.html Motion of Moon Across Sky - moves 13 degrees eastward each day moon will rise 52 minutes later each day Synodic (Lunar) Month - time between two successive new moons: 29.5 days Sidereal Month - time moon takes for one complete orbit of earth: 27.3 days Eclipses Solar Eclipse: - moon blocks out the sun, sun disappears Lunar Eclipse: - moon passes through earth’s shadow - moon no longer visible Conditions for an eclipse: 1. Phase of Moon: Moon must be New or Full Moon 2. Moon must be crossing the ecliptic - must have same declination
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What Causes Eclipses?
What causes eclipses? • The Earth and Moon cast shadows. • When either passes through the other's shadow, we have an eclipse. © 2014 Pearson Education, Inc. Lunar Eclipse © 2014 Pearson Education, Inc. When can eclipses occur? • Lunar eclipses can occur only at full moon. • Lunar eclipses can be penumbral, partial, or total. © 2014 Pearson Education, Inc. Solar Eclipse © 2014 Pearson Education, Inc. When can eclipses occur? • Solar eclipses can occur only at new moon. • Solar eclipses can be partial, total, or annular. © 2014 Pearson Education, Inc. Why don't we have an eclipse at every new and full moon? • The Moon's orbit is tilted 5° to ecliptic plane. • So we have about two eclipse seasons each year, with a lunar eclipse at full moon and solar eclipse at new moon. © 2014 Pearson Education, Inc. Summary: Two conditions must be met to have an eclipse: 1. It must be full moon (for a lunar eclipse) or new moon (for a solar eclipse). AND 2. The Moon must be at or near one of the two points in its orbit where it crosses the ecliptic plane (its nodes). © 2014 Pearson Education, Inc. What have we learned? • Why do we see phases of the Moon? – Half the Moon is lit by the Sun; half is in shadow, and its appearance to us is determined by the relative positions of Sun, Moon, and Earth. • What causes eclipses? – Lunar eclipse: Earth's shadow on the Moon – Solar eclipse: Moon's shadow on Earth – Tilt of Moon's orbit means eclipses occur during two periods each year.
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Lunar Phases and Eclipses
Lunar Phases and Eclipses Created by the Lunar and Planetary Institute For Educational Use Only LPI is not responsible for the ways in which this powerpoint may be used or altered. 1 http://solarsystem.nasa.gov/multimedia/gallery/Earth_Moon.jpg Preliminary Topics Before students can understand the reason for phases, they need to understand: • The Moon orbits the Earth Ecliptic plane • The Moon orbit at an angle with respect Moon’s orbital plane to the Earth’s orbit around the Sun • The Moon doesn’t shine on its own; it reflects sunlight • The scale of the Moon and Earth’s sizes and distance Please go through Earth and Moon statistics before trying to cover the reason for phases or eclipses. 2 Phases: Observing and Identifying New (couple days) Waxing Crescent (several days) 1st Quarter Waxing Gibbous (several days) Full Waning Gibbous (several days) 3rd Quarter Waning Crescent (several days) New 3 http://www.lpi.usra.edu/education/skytellers/moon_phases/about.shtml Phases--Causes • The Sun shines on the Moon. – When the sunlight reflects off the Moon’s far side, we call it a New Moon – When the sunlight reflects off on the Moon’s near side, we call it a Full Moon – Between New and Full, we see parts of the daytime side of the Moon. Golfball and Blacklight Activity 4 Please do NOT use this to teach phases; use to test for comprehension 5 http://starchild.gsfc.nasa.gov/docs/StarChild/questions/question3.html starchild.gsfc.nasa.gov/docs/StarChild/questions/phases.html6 Eclipses • The Sun and Moon occasionally line up so that we have an eclipse.
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