Leeds Astronomical Society LAS Meetings Observing Membership

 

 

M51 - Whirlpool Galaxy

(James Clark 2022 + 2023)
(James Clark 2022 + 2023) Cropped Close-up
(James Clark 2022)
(James Clark 2022) Cropped Close-up
(Ivor Trueman)
(Ivor Trueman)
(Ivor Trueman)
(Ivor Trueman)

Information...

M51 - the Whirlpool Galaxy is called a 'grand-design' spiral galaxy, because of it's prominent and well defined spiral arms. Estimated to be 23 million light-years away, it has a about mass of 160 billion Suns (or about 10% of the mass of the Milky Way) and an estimated diameter of about 76,000 light-years.

The Galaxy's pronounced spiral structure is thought to be due to the interaction with it's companion galaxy NGC 5195, which can be seen at tugging the end of of one of it's arms. The small galaxy has been gliding past the Whirlpool for hundreds of millions of years, with the interaction resulting in a region of new star formation.

One curious aspect about these well defined spiral galaxies, is that the structure of the spiral is thought to be rotating at a slower rate than the material itself. In the density wave theory the visible arms form as the result of gathering interstellar matter. As clouds of hydrogen approach an arm, the arm acts as a gravitational potential well, slowing the gas down & compressing it. We see this effect as dust lanes at the back of the spiral arms. As the cloud is compressed, star formation takes place, resulting in short-lived bright stars which mark the front of the spiral arms. These massive stars, in turn, have the effect of driving apart the clouds through stellar winds & supernova explosions. Hence the material in front of the arm once again resembles that which originally entered the back of the arm, and the cycle continues as the gas continues on to the next spiral arm.

For more info. see the Wikipedia entry.

 

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Map

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Measuring Angles

Hold your arm at full length, then close one eye & use the hand shapes shown above to measure the angular distance between the stars.

(Ain't anatomy wonderful!)

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Apparent Magnitude

The apparent magnitude of a star is a measure of how bright it appears from Earth. The scale was introduced over 2,000 years ago by the Greek astronomer Hipparchus, who grouped stars into six categories. The brightest 20 or so were deemed to be 'first magnitude', slightly dimmer stars 'second magnitude', and so on until the barely visible stars were classed as 'sixth magnitude'.

Later it was recognised that our eyesight, once it has been given time to get used to darkness, has a logarithmic response. i.e. a Mag. 1 star is actually 2.512 times brighter than a Mag. 2 star, or 6.310 times brighter than a Mag. 3 star (2.512 x 2.512 = 6.310).

The six Magnitudes thus corresponds to a 2.5126 difference in brightness or 100x.

Apparent magnitude

Today the scale has now been extended, so that brighter objects can have an apparent magnitude of 0 or even negative. The brightest star Sirius, for example, has an apparent magnitude of -1.44 and the Sun is a whopping -26.74, due to it's close proximity to Earth.