Archive for the ‘Introductory topics’ Category

Lookback time

Tuesday, July 28th, 2009

The universe has a very special feature which is a great advantage to astronomers, and which lets them do something many other scientists can’t: it lets them look back in time.

The feature I’m talking about is the finite speed of light. Everyone knows that light has a speed and that it’s very fast (close to 300,000,000 m/s!), but there are implications to that which it’s easy to miss if you spend most of your life living on a ball a few thousand miles across. Since most signals we get from distant objects are in the form of light rays of some sort - and no signal can travel faster than light anyway - we can’t get information on them instantaneously. When you look into the sky during the day, the sunlight you can see has been traveling from the Sun for over eight minutes. That means that if the Sun were to suddenly explode or disappear (or rather more likely, experience an event like a solar prominence or flare) it would take eight minutes before we had any way of telling.

The fact that the fastest thing in the universe takes eight minutes to cross the distance from here to the Sun highlights just how enormous it is, but eight minutes isn’t really that long in other respects. The Sun looks pretty much the same now as it did eight minutes ago, after all. But the other stars in our galaxy are between 4 and 80,000 light-years away (a light-year being the distance light travels in a year) so the delay is much greater.

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Redshift: the second-most powerful tool in astronomy

Tuesday, May 12th, 2009

Light, like sound, is a wave. Sound waves are caused by vibrations in the air (or another medium) transmitting energy: if you sit at a single point in the path of a wave and measure the pressure of the air, you’ll see it fluctuate up and down as the wave passes. With light the medium is the strength of the electromagnetic field instead of air pressure, but the principle is the same.

A wave progressing: the points at which the blue dot is at its highest are a set of wavefronts.

A wave progressing: the points at which the blue dot is at its highest are a set of wavefronts. The height of the dot could represent local air pressure for a sound wave or local EM field for light.

You can think of a wave as being made of a series of ‘wavefronts’ which are emitted from a source and move along in the same direction. For example, all the points at which the pressure is at a maximum make a set of wavefronts for a sound wave. For a simple wave they all move along in a row, all separated by the same, constant distance. This distance is the wavelength of the wave.

Now imagine that the source of the wave is moving away from you. Between emitting one wavefront and the next it will have moved a little distance, and the second wavefront has slightly further to travel. That means it reaches you later than it would have done otherwise, and the wave gets spread out: its wavelength increases. Move the source towards you instead and the opposite happens: the wavefronts get ’squashed’ together and you see a shorter wavelength.

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Spectra: the most powerful tool in astronomy

Saturday, March 14th, 2009

On the subject of stars, all investigations which are not ultimately reducible to simple visual observations are…necessarily denied to us… We shall never be able by any means to study their chemical composition.

When Auguste Comte wrote that in 1835 it seemed like a fairly safe prediction. Travelling to the stars was out of the question of course, and how could we hope to learn anything about what chemicals they’re formed of simply by looking at their light?

But in the same year Comte was writing, Charles Wheatstone was experimenting with heating metals until they glowed and then feeding the light through a prism. It had been known since Newton that putting white light through a prism gave a rainbow or ’spectrum’; that white light is really made up of all visible colours of light mixed together.

A continuous spectrum, which can be formed by passing white light through a prism.

A continuous spectrum, which can be formed by passing white light through a prism.

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The Universe: a brief tour

Saturday, February 14th, 2009

To start my series of introductory astronomy posts, let’s take a quick tour of the universe and its contents. I’ll cover most of the topics here in more detail later, providing details to fill in this framework.

The Solar System

Let’s begin with the familiar Solar System. The Sun is orbited by four rocky planets (of which Earth is the largest); four gas giant planets all much larger than Earth; and many tiny ‘dwarf planets’, asteroids and comets made of rock and ice. They stretch through space over a diameter of 10 billion or so kilometers, but Earth is pretty near the centre at just 150 million km from the Sun.

The planets to scale

The size of the planets to scale (distances not to scale). Click for a bigger version. Credit: NASA

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