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Star Formation & Molecular Astrophysics at the U of C.

Star Formation and Molecular Astrophysics at the U of C. Spitzer Space telescope image of star Formation in the Rho Ophiuchus Molecular cloud - Image from ASA/JPL-Caltech/L. Allen (Harvard-Smithsonian Center for Astrophysics). What Do We Do? Basically, what we do is to try to understand how stars and planets form. To do this we spend a lot of time studying the Interstellar Medium (ISM) - the gas and dust in between the stars. Why study space gas and dust? For more information.read on!

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Star Formation & Molecular Astrophysics at the U of C. | ism.ucalgary.ca Reviews

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Star Formation and Molecular Astrophysics at the U of C. Spitzer Space telescope image of star Formation in the Rho Ophiuchus Molecular cloud - Image from ASA/JPL-Caltech/L. Allen (Harvard-Smithsonian Center for Astrophysics). What Do We Do? Basically, what we do is to try to understand how stars and planets form. To do this we spend a lot of time studying the Interstellar Medium (ISM) - the gas and dust in between the stars. Why study space gas and dust? For more information.read on!

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Star Formation & Molecular Astrophysics at the U of C. | ism.ucalgary.ca Reviews

https://ism.ucalgary.ca

Star Formation and Molecular Astrophysics at the U of C. Spitzer Space telescope image of star Formation in the Rho Ophiuchus Molecular cloud - Image from ASA/JPL-Caltech/L. Allen (Harvard-Smithsonian Center for Astrophysics). What Do We Do? Basically, what we do is to try to understand how stars and planets form. To do this we spend a lot of time studying the Interstellar Medium (ISM) - the gas and dust in between the stars. Why study space gas and dust? For more information.read on!

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ism.ucalgary.ca

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ISM

http://ism.ucalgary.ca/Star_Formation/ISM.html

What is the Interstellar Medium? The gas is mostly in the form of atomic hydrogen (90%) with the remainder mostly helium (and trace amounts of carbon, oxygen, nitrogen, etc.). The majority of the volume of the Galaxy (about 70%) is filled with this gas but with a very low density (less than 0.001 atoms per cubic centimeter) and a very high temperature (about 1 million degrees! That's why most people think of space as empty - the density is just so low. However, since the Galaxy is enormous, even thes...

2

Star Formation

http://ism.ucalgary.ca/Star_Formation/Star_Formation.html

How do Stars and Planets Form? Of course, these cores are not stationary. They are constantly moving and often slowly spinning. As they collapse, however, they begin to spin faster - much like a figure skater spins faster as he pulls his. Ultimately, the gas in the core becomes so hot (greater than 10,000,000 degrees) that the hydrogen atoms begin to fuse - producing a stable source of energy. At this stage, a star is born!

3

IR Emission

http://ism.ucalgary.ca/Star_Formation/IR_Emission.html

Why do Protostars give off infrared and radio light anyways? The gas in interstellar space that ultimately collapses to form stars is very cold. In some cases only about 10 degrees Kelvin (10 degrees above absolute zero! Therefore, the gas itself is very low energy and is unable to radiate high energy light. The figure below displays what is known as the Planck Function which describes how objects of various temperatures can emit light. Kind of like fingerprinting from a very long ways away! And how does...

4

IR & Radio light

http://ism.ucalgary.ca/Star_Formation/IR_&_Radio_light.html

Why use Infrared and Radio light instead of Visible light (i.e. the light we can see with our eyes)? The same is true of protostars. The radio and infrared radiation emitted by the protostars is allowed to pass through the surrounding cloud of gas and dust in which it forms, whereas the visible light is blocked. The two images below show visible light and infrared light images of a cloud containing a young protostar. Only in the infrared image is the protostar clearly visible.

5

How Often?

http://ism.ucalgary.ca/Star_Formation/How_Often.html

How often are stars born? To answer this question we need to talk about the number of stars born each year or, more accurately, the amount of material (gas and dust) that is converted into stars per year. This is expressed in solar masses per year (one solar mass is equal to the mass of our Sun = 2x10 27. If we turn this around, this mean that throughout the entire Universe, a star is born every 0.0002 seconds (i.e. every 2, 10,000th's of a second)!

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matthijs.vanderwiel.org

Matthijs van der Wiel (ASTRON)

http://matthijs.vanderwiel.org/people.php

Matthijs van der Wiel. These are links to web pages of some astrophysicists whom I know personally, and/or collaborate with, or have worked with in the past. This list is mainly meant for myself to not have to google these people every time I want to find their homepage. Names are ordered alphabetically by family name. StarPlan, Copenhagen, DK. SOFIA, CA, USA). NBIA, Copenhagen, DK). Boston University, MA, USA). Dunlap Institute, Toronto, Canada). MPA, Garching, DE. NBIA, Copenhagen, DK). LERMA, Paris, FR.

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Star Formation and Molecular Astrophysics at the U of C. Spitzer Space telescope image of star Formation in the Rho Ophiuchus Molecular cloud - Image from ASA/JPL-Caltech/L. Allen (Harvard-Smithsonian Center for Astrophysics). What Do We Do? Basically, what we do is to try to understand how stars and planets form. To do this we spend a lot of time studying the Interstellar Medium (ISM) - the gas and dust in between the stars. Why study space gas and dust? For more information.read on!

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