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ASTR 1040 ASTR 1040 AccelAccel AstroAstro:: Stars & GalaxiesStars & Galaxies

Prof. Prof. JuriJuri ToomreToomre TA: Nicholas NelsonTA: Nicholas NelsonLecture 19 Tues 15 Mar 2011Lecture 19 Tues 15 Mar 2011

zeus.colorado.edu/astr1040zeus.colorado.edu/astr1040--toomretoomre

SuperbubbleSuperbubbleNGC 3079NGC 3079

Today in Milky WayToday in Milky Way

•• Look at components of galaxy:Look at components of galaxy: stars, gas, duststars, gas, dust

•• Examine the Examine the rotation curve rotation curve of our galaxy, and the of our galaxy, and the unseen mass unseen mass (dark matter) (dark matter) that it impliesthat it implies

•• Look at why Look at why spiral patterns are made in the diskspiral patterns are made in the disk of of galaxies, including our owngalaxies, including our own

•• Examine theExamine the StarStar--GasGas--Star Cycles Star Cycles working in our working in our galaxy disk, and its ingredientsgalaxy disk, and its ingredients

•• Interstellar Medium (ISM) Interstellar Medium (ISM) –– gas and dust, plusgas and dust, plussupersuper--bubblesbubbles blown by multiple supernovaeblown by multiple supernovae

•• RecyclingRecycling on a grand scale, and building the on a grand scale, and building the heavier atoms heavier atoms

TodayToday

•• Homework Set # 8.5Homework Set # 8.5 passed out today, passed out today, HW # 8 dueHW # 8 due

•• Complete your reading ofComplete your reading of 19.4 Mysterious 19.4 Mysterious Galactic CenterGalactic Center

•• Remember that Remember that Planet FinderPlanet Finder project is project is due this due this ThurThur

•• Graded Graded MidMid--Term Exam 2Term Exam 2 will be returned will be returned on on ThurThur

CygnusCygnusXX--11

Observing a Observing a black hole:black hole:

Cygnus Loop SNR Cygnus Loop SNR –– Home of Home of CygCyg XX--11 Cygnus XCygnus X--11: : Blue supergiantBlue supergiant (strong winds) (strong winds) pours H + He onto pours H + He onto accretion disk of black holeaccretion disk of black hole

Blue supergiantBlue supergiant

Accretion diskAccretion disk

StellarStellar--sizesizeblack holeblack hole

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Views of Views of ““Veil NebulaVeil Nebula””

Such SNR maySuch SNR mayhave a BH lurking!have a BH lurking!.. but not this one.. but not this one

SS 433SS 433

top candidatetop candidatefor wild object!for wild object!

another another stellarstellar--size size black holeblack hole

SS 443SS 443

BH + jetsBH + jets

Clicker Clicker –– Size of Black HoleSize of Black Hole•• What does the What does the Schwarzschild radiusSchwarzschild radius of a of a

black hole (BH) depend on?black hole (BH) depend on?

•• A.A. Both mass and chemical composition Both mass and chemical composition of the BHof the BH

•• B.B. Radius of BH, as measured by careful Radius of BH, as measured by careful observations of its sizeobservations of its size

•• C.C. Only the mass of BHOnly the mass of BH

•• D.D. Whether BH formed in massive star Whether BH formed in massive star supernova or in some other waysupernova or in some other way

C.C.

GammaGamma--Ray BurstsRay BurstsHYPERNOVAHYPERNOVA ? ? Collapse of very Collapse of very massive star > BH massive star > BH

Luminosity ~ 10Luminosity ~ 106 6 to 10to 103 3

times output from galaxytimes output from galaxy

Visible from across the Visible from across the universe ! universe !

HSTHST

Now toNow to Our Milky Way GalaxyOur Milky Way Galaxy

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The Milky WayThe Milky Way (fuzzy ribbon of (fuzzy ribbon of light across the sky)light across the sky)

SizeSize of Milky Wayof Milky Way

•• 200200--400400 billionbillion starsstars

•• 100,000 light years 100,000 light years in in diameterdiameter, or, or

~ 30,000 pc = ~ 30,000 pc = 30 30 KpcKpc(kilo(kilo--parsecs)parsecs)

•• SunSun is located about is located about 8.5 8.5 kpckpc from center, from center, in the `Orion Armin the `Orion Arm’’

ArtistArtist’’s sketch!s sketch!

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REMINDERREMINDER

If If wewe might see might see Milky WayMilky Way from outside from outside

Spiral Spiral SbSb galaxygalaxyNGC 4414NGC 4414

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We mightWe might preferprefer to look like this! Prettier?to look like this! Prettier?

M101M101with morewith moredistinctivedistinctivespiral armsspiral arms

Composite of M101 Composite of M101 –– much goes on!much goes on! Milky Way Anatomy: Spiral GalaxyMilky Way Anatomy: Spiral Galaxy

•• DiskDisk:: includes includes spiral armsspiral arms ----young, new star young, new star formationformation

•• Bulge & HaloBulge & Halo::older stars, older stars, globular clustersglobular clusters

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Clicker Clicker –– Where are we?Where are we?

•• Why was it so difficult to figure out Why was it so difficult to figure out where in the where in the Milky WayMilky Way are the Sun and Earth located, and if are the Sun and Earth located, and if ours is the only ours is the only ““nebulanebula”” (galaxy) ?(galaxy) ?

•• A.A. We are immersed in a soup of stars, gas and dust, so hard to see far

•• B.B. In a middle of city of stars, hard to figure shape of overall `metropolitan area’

•• C.C. Gas and dust can absorb light, making distance estimates uncertain

•• D.D. All of the above

D.D.

Disk is very thin!Disk is very thin!

ArtistArtist’’s edges edge--on viewon view

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Spiral galaxy Spiral galaxy NGC 891NGC 891 –– nearly edgenearly edge--onon

stars, gas, dust in diskstars, gas, dust in disk

OneOne--pager:pager:ALL about us!ALL about us!

SketchSketchof Milky Wayof Milky Way

EdgeEdge--onon

TopTop

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PrePre--Milky Way: early halo + disk Milky Way: early halo + disk

How to build a How to build a spiral galaxyspiral galaxy

(or so we think!)(or so we think!)

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The Star-Gas-Star Cycle

Cycle ofCycle ofstarstar gas gas starstar

All spiral galaxiesAll spiral galaxiesare constantly changingare constantly changing

Inventory ofInventory of““stuffstuff”” makingmakingup our galaxyup our galaxy

Stars Stars

Gas Gas

DustDust+ + ““darkdarkmattermatter””

Many views of our galaxy diskMany views of our galaxy diskReading clicker Reading clicker –– mapping our galaxymapping our galaxy

•• We want to map the We want to map the structures of very cold structures of very cold gas within the dusty diskgas within the dusty disk of the Milky Way. of the Milky Way. What wavelengths should we be using, What wavelengths should we be using, and why?and why?

•• A.A. radioradio•• B.B. visible lightvisible light•• C.C. xx--raysrays

A.A.

A.A. RadioRadio•• DustDust obscuresobscures our our

vision of much of the vision of much of the galaxy in visible and galaxy in visible and UV light.UV light.

•• XX--rays only highlight rays only highlight the hottest and the hottest and weirdest placesweirdest places

•• 21 cm radio waves21 cm radio wavesmap normal hydrogen map normal hydrogen gas gas ---- these pass these pass through dust unaffectedthrough dust unaffected

confused visible imageconfused visible image

MW disk in radioMW disk in radio

Motion of stars in spiral galaxyMotion of stars in spiral galaxy

Disk:Disk:circular +circular +bit up/downbit up/down

Halo & bulge:Halo & bulge:swarming in swarming in and outand out

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DifferentDifferentstar motionsstar motionsin disk & haloin disk & halo

1.1.

2.2.

MMRR = R = R xx V V 22 / G/ G

Stars moving in circles: orbital velocity lawStars moving in circles: orbital velocity law

massmassinwardinward

radiusradius orbitalorbitalvelocityvelocity

……faster orbit,faster orbit,more massmore mass

MW rotation curveMW rotation curve

solar systemsolar system

Massive dark matter halo for MWMassive dark matter halo for MW

•• Stars and gas are Stars and gas are embedded in a embedded in a much larger much larger dark dark matter halomatter halo ????

•• DonDon’’t know what t know what dark matter is dark matter is yetyet…… probably probably not not baryonic baryonic (usual (usual protons, neutrons, protons, neutrons, electrons)electrons)

Reality for the Milky WayReality for the Milky Way•• Rotation curve is flat Rotation curve is flat

or even rising!or even rising!

•• Most of the mass of Most of the mass of the galaxy is outside the galaxy is outside the solar circle!the solar circle!

•• But few stars, little But few stars, little gas theregas there……

•• DARK MATTERDARK MATTER ! ! probably in large probably in large halo halo ---- outweightsoutweightsstars+gasstars+gas by factorby factorof 3 to 10 of 3 to 10

Role of dark matter on rotation profileRole of dark matter on rotation profile

DARK MATTERDARK MATTER

Dark matter halo for galaxiesDark matter halo for galaxies•• Presence revealed Presence revealed

by by rotation curvesrotation curves(motions of stars in (motions of stars in galaxy)galaxy)

•• Dark matter extends Dark matter extends beyond visible part of beyond visible part of the galaxythe galaxy ---- mass is mass is ~10x~10x stars and gas !stars and gas !

•• Most likely subatomic Most likely subatomic particles, as yet particles, as yet unidentified (unidentified (weakly weakly interacting massive interacting massive particles particles –– WIMPsWIMPs ?? ))

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Discussion TopicDiscussion Topic

““Cycle of Stars and GasCycle of Stars and Gas””---- Does this continue forever in Milky Way Does this continue forever in Milky Way ––

why or why not? And does it depend on your why or why not? And does it depend on your location within MW? location within MW?

Why spiral arms?Why spiral arms?

““Density wavesDensity waves”” ––stars move in and stars move in and out of denser out of denser regionsregions

More like More like ripples in a ripples in a pondpond than arms of than arms of a pinwheela pinwheel

In dense regions, In dense regions, star star formation is more formation is more intenseintense, so , so ““armsarms””are brighterare brighter M51 M51 -- WhirlpoolWhirlpool

Gas/starsGas/stars are pulled are pulled a little a little forward or forward or backwardbackward toward toward the high density the high density regionsregions

Such clumping helps Such clumping helps create a spiral create a spiral patternpattern

Push and pullPush and pull ofofgravity in diskgravity in disk