Welcome to Harvard Astronomy 201b · 2013-01-29 · Demonstrations, iBooks Author, Javascript,...

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Welcome to Harvard Astronomy 201b Alyssa Goodman 160 Concord Avenue, Room 330 Office: 617-495-9278 SMS: 617-230-7080 [email protected] www.cfa.harvard.edu/~agoodman Chris Faesi [email protected] 60 Garden Street, P-301 v.2013 Nathan Sanders [email protected] 60 Garden Street, A-112

Transcript of Welcome to Harvard Astronomy 201b · 2013-01-29 · Demonstrations, iBooks Author, Javascript,...

Page 1: Welcome to Harvard Astronomy 201b · 2013-01-29 · Demonstrations, iBooks Author, Javascript, Python (required) write up of special topic background & module explanation, placed

Welcome to Harvard Astronomy 201b

Alyssa Goodman160 Concord Avenue, Room 330

Office: 617-495-9278SMS: 617-230-7080

[email protected]/~agoodman

Chris [email protected] Garden Street, P-301

v.2013

Nathan [email protected] Garden Street, A-112

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What is out there?

Where is it?

What is it doing?

How do we find out?

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What does Wikipedia say is in the ISM?

but that’s NOT all--should we fix it?

What about: cosmic rays? dust? magnetic fields? photons?It’s really not just gas.

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Our fundamental understanding of the ISM & Star Formation hasn’t been fully transformed in the past decade but teaching and learning have been...

ISM: evidenceprobes

star birth: evidence_effects

ISM "phases"

photons (radiation)

"turbulence"

magnetic fields

atomic and molecular gas

dust

stellar evolution: evidence

star death: evidence_effects

IGM: evidence

emission_absorption of spectral

Iines

radiative transfer

non-thermal

processes

probes of temperature

magneto-hydro-

dynamicshydro-

dynamicsradiation pressure

winds_jets: evidence_effects

dark matter: evidence

chemistrythermo-

dynamics (heating/cooling)

probes of composition

probes of density

probes of velocity

probes of magnetic fields

galactic structure: evidence

shock physics instabilities

virial theorem equilibria

excitation/ ionization

solid state processes

SED modeling

spec-troscopy

(high-D) imaging

disk formation_fragmenta-

tion

numerical simulations

distribution measures_theorems

cosmic rays

polarimetry

thermal emission (black-body)

scattering extinction

Student Work in Harvard Astronomy 201b

Assigned “problem sets” Background

Reading in Required Text

Journal Article Discussion

(1 per week)

10 minute in-class presentation of

working online module (with

demo & discussion, 20% of

course grade)

prior to February 14 week of February 18-22 after February 25

"development" workshops during class

time on WorldWide Telescope, Wolfram

Demonstrations, iBooks Author, Javascript, Python

(required)

write up of special topic background & module explanation,

placed online (15% of course

grade, edX for best)

by May 3

Student topical

research

consult with AG (and TFs as-needed) to discuss draft module plan

(Fridays at 10)

choose one special

topic for in-class & online presentations

choose one article for in-class &

online summary

after consultation with TFs, post online article

summary (5% of course grade)

lead in-class discussion, of

article, considering advance & live questions (30

minutes, 10% of course grade)

4 problem sets (students can consult, but

solutions should be original; 10% of course

grade per set)

when it's not your turn: submit 2

questions about week's article(s),

(each week, 5% of course grade total)

on January 30 5 PM Tuesday before discussion

revise/finalize post summarizing article (in consultation with TFs)

place on course site (some to astrobites & Sky & Tel/blog, 5% of course grade)

Thursday of discussion by 1 week after discussion

roughly every 2.5 weeks throughout the term

passages in Draine's book will be suggested,

and additional reading will be

distributed online and in-class as well

v.2013

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AG’s CurrentResearch Portfolio

http://www.cfa.harvard.edu/~agoodman/

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Points of View• Barnard’s Ophiuchus on flickr, WWT• Stromgren Spheres on Wikipedia• Stromgren Sphere on the Blackboard (and in a Google Spreadsheet)• Numerical Simulations of HII regions• Hope Chen’s Research Exam...(COMPLETE, wtml demo)

Student Work in Harvard Astronomy 201b

Assigned “problem sets” Background

Reading in Required Text

Journal Article Discussion

(1 per week)

10 minute in-class presentation of

working online module (with

demo & discussion, 20% of

course grade)

prior to February 14 week of February 18-22 after February 25

"development" workshops during class

time on WorldWide Telescope, Wolfram

Demonstrations, iBooks Author, Javascript, Python

(required)

write up of special topic background & module explanation,

placed online (15% of course

grade, edX for best)

by May 3

Student topical

research

consult with AG (and TFs as-needed) to discuss draft module plan

(Fridays at 10)

choose one special

topic for in-class & online presentations

choose one article for in-class &

online summary

after consultation with TFs, post online article

summary (5% of course grade)

lead in-class discussion, of

article, considering advance & live questions (30

minutes, 10% of course grade)

4 problem sets (students can consult, but

solutions should be original; 10% of course

grade per set)

when it's not your turn: submit 2

questions about week's article(s),

(each week, 5% of course grade total)

on January 30 5 PM Tuesday before discussion

revise/finalize post summarizing article (in consultation with TFs)

place on course site (some to astrobites & Sky & Tel/blog, 5% of course grade)

Thursday of discussion by 1 week after discussion

roughly every 2.5 weeks throughout the term

passages in Draine's book will be suggested,

and additional reading will be

distributed online and in-class as well

v.2013

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astrometry.net

[published 1927]

“Barnard’s” Ophiuchus in 2013

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20 cm VLA from MAGPIS (Helfand et al. 2006) & MIR from Spitzer GLIMPSE (see Churchwell et al.)3.6, 4.5, 8.0, 20cm (Luptonized, see Lupton et al. 2004)

image “height” is 1.6 degrees (e.g. 140 pc at 5 kpc)

radio SNR

warm dust cold dust

HII regions(+SNR)

Massive Star-Forming Regions

What Stars can do to the ISM

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Evolution of an HII Region in a Turbulent Medium

from S.J. Arthur 2007

back mid-plane front

80,000 yr

209,000 yr

black =105 cm-3

white = 10 cm-3

black = 0 Kwhite = 104 K

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Tasting “M17”...

Synthetic [OIII], H and [NII] emission-line image from a 5123 numerical simulation: Mellema, Henney, Arthur & Vàzquez-Semadeni 2009

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What now?All

make sure your name/email is on the course sign-up listfill out online survey (on course web site) by this eveningread Barnard’s article by Thursday

One Volunteerlead discussion of Barnard’s article Thursday

AGrefine Journal Article & Topics list to optimize for student backgrounds