The INTERSTELLAR MEDIUM The ISM is all the stuff between stars; it’s about 10% of the mass in the galaxy. It is also the stuff (gas and dust): from which stars are born and into which they throw off their outer parts when they die.

The ISM is Important NGC 604, w/ 200 young stars The gas between stars is of VERY low density, with the densest ISM clouds far less dense the best lab vacuum Nonetheless, it is from these gas clouds that new stars are born. Old stars expel large portions of their envelopes into the ISM. Heavier elements, which are cooked via nuclear fusion in stellar interiors, enrich (or pollute) the ISM.

Dimming and Reddening Light traveling through these clouds will be absorbed and reddened (more blue light absorbed or scattered), so star light looks different than it did when emitted. Black in center, redder at edges of dense clouds Astronomers use spectral lines to “de-redden” a star’s light and can figure out its real brightness and distance.

Dust is Heated and Radiates Young stars give off visible and UV light which heats dust in the surrounding dense cloud The dust gives this heat back as IR light The stars are often invisible because of absorption Only the warm dust and the gas near it may be seen Dense cloud with embedded stars applet

Light Polarized by Dust Scattering Dust particles < 1m in size, made of C, O, Si, Fe If the molecules or dust grains are not spherical and are aligned, then light is polarized: E vectors (mostly) in one plane Magnetic fields can align dust grains (which have some iron in them) So mapping polarized light yields directions of magnetic fields in ISM

When starlight passes through interstellar dust It gets fainter The blue light tends to scatter sideways while the red continues to us Wavelengths all get longer (redder) All of the above #1 and #2

When starlight passes through interstellar dust It gets fainter The blue light tends to scatter sideways while the red continues to us Wavelengths all get longer (redder) All of the above #1 and #2

PHASES OF THE INTERSTELLAR MEDIUM The cooler parts of the ISM are NEUTRAL. The hotter parts are IONIZED (some electrons ripped off atoms). The neutral phases include: Molecular clouds, mainly made of H2 molecules. From these new stars form, but they make up a small portion of the mass of the ISM and an even smaller portion of the volume. Atomic (H I) clouds and diffuse gas. These diffuse phases make up the bulk of both the mass and volume of the ISM.

IONIZED ISM PHASES H II regions: parts of molecular clouds which are ionized by hot, young (O or B) stars, which pump out lots of powerful UV photons -- these are spectacular, but rare. Shock heated ISM -- very low density -- makes up a big part of the volume, but only a small part of the mass of the ISM --mainly heated by Supernovae --sometimes called the galactic corona

CLOUDS or NEBULAE AS OBSERVED IN THE VISIBLE BAND 1. Dark Nebulae = Molecular Clouds: dust absorbs nearly all the visible light from stars behind the clouds so they look black on the sky. Rho Ophiuchi (left), Antares (right) in V and IR

2. Bright Nebulae Emission Nebulae a.k.a. H II regions O or B stars (w/ lots of UV photons) ionize gas. We see recombination emission lines, mainly from: O II, N II, and N III in red, pink and blue number density, n, at least 100 cm-3 (to 1000 cm-3) temperature, T~104 K (8,000 to 12,000 K) Reflection Nebulae Dust scattering light near stars; Since dust preferentially scatters blue light, these nebulae look blue.

Milky Way with Dusty ISM Emission nebulae; Plane of MW is dashed line

Emission Nebulae: M8 & M20(Trifid) Dust lanes trisect the emission nebula on the right Blue regions are refection nebulae Jet from protostar at lower left (about 0.5 pc long)

Nebula Structure & Spectrum

Bright Nebulae (continued) C. Planetary nebulae Shells of gas ejected from old stars; Ionized by hot core of the star (will become a WD); Usually look ring-like because of greater column depth of emitting gas along edges of shell rather than through core (Chapter 20) D. Supernova Remnants Lots of mass, blasted out at high velocities during the deaths of massive stars (Chapter 21). Seen in X-ray and radio bands as well as in visible. Fade after only about 100,000 years and supernovae are pretty rare events to begin with.

Planetary Nebulae Cat’s Eye, Eskimo, Helix, & M2-9 PNs.

Supernova Remnants Start on the next slide on 9/29 N132D & Crab SNRs

Results of First Exam Mean before curve: 54.37 Curve: +20 Mean after curve: 74.37 Standard deviation: 13.07 Distribution: ≥90: 5 (high = 100) ≥80: 11 ≥70: 11 ≥60: 14 <60: 9 (low=50; <52 = random guessing: 2) Start here on 9/29/09

Most Difficult Questions Q4: False, INVERSELY proportional: E=hc/ Q12: False:M=2x1033g or 2x1030 kg Q16: False: mass 4He < 4(mass 1H) Q19: False: 1 pc = 3.11013km=3.11016m Q30: D: f = c/ = 3.00x108m s-1 / 3.00x103 nm = 3.00x108m s-1 / 3.00x10-6 m = 1.00x1014 Hz Q31: C: E=hf=(6.610-34J•s)(2.01021Hz) = 13.2 10-13 J = 1.3 10-12 J Q36: A: LC/LD = 4 RC2TC4/ 4 RD2TD4 = (RC/RD)2(TC/TD)4=(42)(6/4)4=16(3/2)4=16(81/16)

Last Difficult Questions Q45: B (Vr/c)=(obs- em)/ em =0.02nm/400.0nm=2x10-2/4x102=0.5x10-4. So Vr=(3.00x105km/s)(5x10-5) = 15 km/s Q46: D: Since Washo has a negative apparent magnitude it must be very bright: m = 6.5-(-0.5) = 7 = 5+2, so the factor by which Washo exceeds Hadun in brightness is: 100  (2.512)2 = 631 Q50: B, the ratio of the stars’ masses: A double-line-spectroscopic binary that is ALSO eclipsing or visual (or interferometric) gives the individual masses as the latter types of binaries give the SUM of the masses.

SUMMARY OF ISM CONDITIONS (in order of decreasing T) SHOCK HEATED (or coronal gas): Highly ionized T between 105 and 106 K n between 10-4 and 10-3 cm-3 About 1 percent of ISM mass About 1/2 of ISM volume first found only in 1970s via UV absorption lines and later by X-ray emission H II REGIONS: Moderately ionized 8000 K < T < 12,000 K 100 < n < 1000 cm-3 very small fraction of ISM mass and volume detected via optical emission lines and radio lines Start here on 9/29

HII Regions around Hot Stars M16: (left) Eagle Nebula; (top) Pillars of cold gas in M16 M8: (right) Lagoon Nebula; (top) Core of M8: Hourglass

Cooler ISM Phases WARM INTERCLOUD MEDIUM: In the old days this was considered to be the bulk of the ISM and it is still the dominant/average constituent: partially ionized --1000 < T < 8000 K ; 0.01 < n < 0.1 cm-3 --Roughly half of both mass and volume of ISM --detected via 21 cm radio and UV absorption lines ATOMIC CLOUDS: mostly neutral H, in atomic, or H I, form --50 < T < 150 K; 1 < n < 100 cm-3 --roughly 1/2 of ISM mass but only about 1 percent of ISM volume --Found first of all ISM constituents: via visble abs. lines; later, UV abs found and most easily mapped via 21-cm emission from H I Start here on 10/4

Absorption Lines from ISM Clouds Extra, narrow absorption lines are added to a star’s spectrum by intervening ISM clouds: at different redshifts

21 cm Emission from H I If protons and electrons have parallel spins the energy is slightly greater than when their spins are anti-parallel; the spontaneous spin-flip gives off photons w/ = 21 cm.

Pop Quiz Print your name. (1) Sketch a LABELED H-R diagram (either spectral type or temperature and either luminosity or absolute magnitude), (5) Note the Main Sequence, Sun, Red Giants, Supergiants and White Dwarfs on your H-R diagram. (5) Start here on 2/20

The COLDEST Phase DARK (MOLECULAR) CLOUDS: mostly molecules of H2 , then He, CO, OH, CO2 , H2O, etc. some much heavier molecules, e.g., alcohol, formaldehyde, even amino acids are present, though much rarer contains most of the dust grains that redden and absorb starlight 8 < T < 50 K 102 < n < 105 cm-3 less than 1 percent of ISM mass and volume

MOLECULES HAVE RICH SPECTRA In addition to the electron energy levels that single atoms have, when combined in molecules: there are quantized rotational energy levels; there are quantized vibrational energy levels. Both of these lead to lots of spectral lines, mostly in the IR, mm (or microwave) and radio bands. Thus even rare molecules in space can be detected by tuning telescopes to particular frequencies corresponding to these rotational/vibrational transitions.

If gas and dust in space are dark, how do we know they are there? We sometimes see absorption lines from interstellar gas Infrared telescopes can see cool dust Radio telescopes detect interstellar gas All of the above We can’t really be sure. Space may be empty.

If gas and dust in space are dark, how do we know they are there? We sometimes see absorption lines from interstellar gas Infrared telescopes can see cool dust Radio telescopes detect interstellar gas All of the above We can’t really be sure. Space may be empty.

Molecular Rotational Transition in Formaldehyde (H2CO)

Molecular Lines Near M20 Most formaldehyde is found in the darkest, densest part of the molecular cloud

Molecular Lines Yield Cooling Clouds can stay cool, even if collapsing, if all generated radiation can escape Heat, or random collisions, excite rotational-vibrational levels Photons emitted from them, esp. CO, keep clouds cool and cloud could keep contracting Until: density gets so large that these mm and IR photons are absorbed many times before escaping. Then the temperature will rise and gas pressure goes up rapidly. This is a key process in star formation!