Send the link below via email or IMCopy
Present to your audienceStart remote presentation
- Invited audience members will follow you as you navigate and present
- People invited to a presentation do not need a Prezi account
- This link expires 10 minutes after you close the presentation
- A maximum of 30 users can follow your presentation
- Learn more about this feature in our knowledge base article
Do you really want to delete this prezi?
Neither you, nor the coeditors you shared it with will be able to recover it again.
Make your likes visible on Facebook?
You can change this under Settings & Account at any time.
The life cycle of a star
Transcript of The life cycle of a star
The lower on the scale, the brighter the star. Magnitude scale if stars were 3.26 light years away (difference of distance is not taken into account) = absolute magnitude H - R diagram Stars emit energy In short Birth of star Death Our real ancestor Light is received through prism
Spectrum is formed
Spectrum can be analysed
Conclusions about the composition and conditions of a star The capturing and anlysing of a specturm Spectroscopy allows the determination of the composition and conditions of a star process Composition Conditions Presence of different elements in a star each element has a unique signature This signature can be identified in the spectrum of a star every different element absorbs a different part of the wavelength The emission lines can tell temperature, luminosity and velocity This has to do with the strength of absorption, which is dependant on temperature Concluded in a table.... stars range in size from 20 km to 0.9 billion km stars appear to us as points of light The human eye is relatively insensitive to colours of point sources The visible diameter of stars is nearly zero Energy is produced by fusion of hydrogen into helium ('hydrogen burning') Stars lose energy (and Hydrogen) surface temperature luminosity surface temperature luminosity surface temperature luminosity surface temperature blue giant (high mass) red supergiant neutron star yellow dwarf (lower mass) red giant white dwarf brown dwarf All hydrogen is gone gravity contracts the star No hydrogen fusion possible temperature increases helium fusion is possible expansion the same story, no hydrogen, it expands Duration !!The whole life cycle of a star is decided by its mass!! Lower mass = yellow dwarf Larger mass = blue giant nebula gravity due to mass contraction causes heat heat makes hydrogen burning possible Rest of loose matter is either blown away or forms planets usually referred to as the birth of the star A cloud of dust and gas Hydrogen runs out Gravity contracts the star Increased temperature allows helium fusion Helium runs out Star continuous to fuse until all iron has ran out less than 4 solar masses greater than 4 solar masses higher mass lower mass red gaint forms planetary nebula and becomes white dwarf Red supergiant experiences supernova. Eventually becomes neutron star or black hole is formed Planets are made of the gasses and dust in the nebula Nebulae are formed when lower mass star dies We are made of the gasses and dust from the nebula supernova observed by hubble