Astronomy 1 Fall 2014 Lecture 2; October 7, 2014 UCSB Astro 1 -
Martin Set your alarm clock for 3am to see tonights eclipse!
Slide 2
Previously on Astro-1 Goal 1 The big picture The Universe is
huge; we will make a Grand Tour Goal 2 The scientific method
Demarcation: what is science? Falsification: how do you test
scientific theories? Corroboration: what is a good scientific
theory? Goal 3 Learning scientific language Science terms have very
precise definitions, with sometimes somewhat different meaning than
in the current language (e.g., Powers of ten; Units;Small Angle
Formula) UCSB Astro 1 - Martin2
Slide 3
Today on Astro-1 Constellations & Celestial Sphere Seasons
The moons orbit Lunar eclipses Solar eclipses Ancient studies of
moon and suns orbit UCSB Astro 1 - Martin3
Slide 4
The Night Sky UCSB Astro 1 - Martin4
Slide 5
The sky is divided into 88 constellations, but the stars are at
different distances UCSB Astro 1 - Martin5
Slide 6
6
Slide 7
7
Slide 8
The diurnal (daily) motion of the stars. UCSB Astro 1 -
Martin8
Slide 9
The diurnal (daily) motion of the stars. UCSB Astro 1 -
Martin9
Slide 10
The night sky changes during the year How fast does the
position of the Earth move around the sun every month? UCSB Astro 1
- Martin10
Slide 11
The imaginary celestial sphere. The celestial equator and poles
are projections of the Earths axis of rotation out into space. UCSB
Astro 1 - Martin11
Slide 12
UCSB Astro 1 - Martin12
Slide 13
Seasons UCSB Astro 1 - Martin13
Slide 14
UCSB Astro 1 - Martin14
Slide 15
UCSB Astro 1 - Martin15
Slide 16
Ecliptic plane: the plane in which the Earth moves around the
Sun. UCSB Astro 1 - Martin16
Slide 17
Ecliptic plane and the ecliptic: just a matter of perspective
UCSB Astro 1 - Martin17
Slide 18
UCSB Astro 1 - Martin18
Slide 19
UCSB Astro 1 - Martin19
Slide 20
UCSB Astro 1 - Martin20
Slide 21
UCSB Astro 1 - Martin21
Slide 22
Midight Sun from Arctic Circle UCSB Astro 1 - Martin 22 What
direction is the photographer facing? A.North B.South C.East D.West
E.None of the above. This photograph was photoshopped.
Slide 23
The Moons Orbit UCSB Astro 1 - Martin23
Slide 24
This picture of the Earth and the Moon was taken in 1992 by the
Galileo spacecraft on its way toward Jupiter. UCSB Astro 1 -
Martin24
Slide 25
What you see from earth UCSB Astro 1 - Martin25
Slide 26
When do you see the moon in the morning sky? UCSB Astro 1 -
Martin26
Slide 27
UCSB Astro 1 - Martin27
Slide 28
Sidereal month: the time the Moon takes to complete one full
revolution around the Earth with respect to the background stars:
27.32 days Synodic (lunar) month: Time from one new moon to the
next: 29 days. UCSB Astro 1 - Martin28
Slide 29
Why dont we have eclipses every month? UCSB Astro 1 -
Martin29
Slide 30
UCSB Astro 1 - Martin30
Slide 31
Lunar eclipse: Moon is in the shadow of the Earth UCSB Astro 1
- Martin31
Slide 32
Lunar eclipse: three types UCSB Astro 1 - Martin32
Slide 33
The Moon moving through the Earths umbra over 3 hours. UCSB
Astro 1 - Martin33
Slide 34
On average, two or three lunar eclipses occur in a year. Of all
lunar eclipses, roughly one-third are total, one-third are partial,
and one-third are penumbral.
Slide 35
Tonights Eclipse UCSB Astro 1 - Martin35
Slide 36
How did ancient astronomers discover that the Earth is round?
UCSB Astro 1 - Martin36
Slide 37
Solar eclipse UCSB Astro 1 - Martin37
Slide 38
A total solar eclipse. The moon passes in front of the sun.
UCSB Astro 1 - Martin38
Slide 39
UCSB Astro 1 - Martin39
Slide 40
UCSB Astro 1 - Martin40
Slide 41
During a total solar eclipse, the tip of the Moons shadow
traces an eclipse path across the Earths surface. People within the
eclipse path see a total solar eclipse as the tip moves over them.
Anyone within the penumbra sees only a partial eclipse. Photo from
Russian space station Mir (of same eclipse in previous 2 slides)!
UCSB Astro 1 - Martin41
Slide 42
UCSB Astro 1 - Martin42
Slide 43
Annular solar eclipse. UCSB Astro 1 - Martin43
Slide 44
There are at least two, but never more than five solar eclipses
each year.
Slide 45
UCSB Astro 1 - Martin45
Slide 46
Eratostheness determined the diameter of the Earth around 200
B.C.! Distance from Alexandria to Syene was said to be about 5000
stades, so Earths circumference was computed to be 50 5000 =
250,000 stades UCSB Astro 1 - Martin46
Slide 47
Aristarchus determined distances to sun and moon, and
determined sizes of moon and sun relative to Earth around 280 B.C.!
He got the answer wrong because of poor measurements, but had the
right technique. UCSB Astro 1 - Martin47
Slide 48
Slide 49
Summary The night sky Seasons Why is it colder in winter? Lunar
Phases: How do they arise? Length of the Month: How long does it
take for the moon to go around the Earth? The Moons Orbit: Why dont
we have lunar eclipses every month? Solar eclipses What kind of
solar eclipses are there? When do they happen? UCSB Astro 1 -
Martin49
Slide 50
Homework Due 10/13/14 On your own: answer all the review
questions in chapter 2-3. To TAs: answer questions 2.40, 2.46,
3.31, 3.43 UCSB Astro 1 - Martin50