Getting the Measure of the Universe Dr. Martin Hendry Glasgow University.

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Presentation transcript:

Getting the Measure of the Universe Dr. Martin Hendry Glasgow University

Ptolemy: 90 – 168 AD

Nicolaus Copernicus 1473 – 1543 AD

Retrograde motion of Mars

Earth Sun Venus We can use Pythagoras’ theorem!!

Solar Eclipses Total Eclipse Zone only about 20km across, but sweeps over many countries as the Earth spins

Tycho Brahe: 1546 – 1601 AD

Kepler’s laws, published 1609, 1619

Galileo Galilei: 1564 – 1642 AD Galilean Moons: 1610

Isaac Newton: 1642 – 1727 AD The Principia:

Nowadays we can use radar: Distance = Speed x Time

Nowadays we can use radar: Distance = Speed x Time But what is the speed of light?…

Light waves

Wavelength Frequency = No of waves produced per second Light waves

Wavelength Frequency = 2450 MHz = 2450 Million waves per second Light waves

Wavelength Speed = 2450 million wavelength Light waves

Light travels 300,000 km every Second…… ……That’s about 10 million, million kilometres every year!!!

The stars are VERY far away. The nearest star (after the Sun) is about 40 million million km from the Earth. It takes light more than 4 years to travel this distance. If the distance from the Earth to the Sun were the width of this screen, the next nearest star would be in Rome.

Measuring Astronomical Distances: Parallax

Even the nearest star shows a parallax shift of only 1/2000 th the width of the full Moon

Spectroscopy

What can we learn from spectra?

Absorption e -

Emission e -

Wobbly stars: the key to finding extra-solar planets Planets and stars orbit their centre of mass Planets are too faint to see directly - so stars wobble but

The Sun’s “wobble”, due to Jupiter, seen from 30 light years away = width of a 10p coin in Madrid

Doppler Shift

Star Laboratory

51 Peg – the first new planet

So we can use spectra to tell what stars are made of….. ……If those stars have planets, we can also use spectra to find them, and tell what gases are in their atmospheres!