Collisional Ionization

Computed fractional ionization degree for iron in as function of gas temperature

Slide 4-1

Photonionization-structure for spherical nebulae

H and He for an O and B star He and O for a planetary nebula Slide 4-2

Interstellar polarization

Interstellar polarization for stars in the Milky Way in Galactic coordinates. The interstellar magnetic field is predominantly parallel to the disk.

Slide 4-3

Dust in the IR-galaxy M82

stellar continuum emission

dust continuum emission

narrow PAH emissions

SiO absorption 9.7μm

Slide 4-4

Magnetic fields in M51

Structure of the magnetic field derived from the polarization of the synchrotron radiation

Slide 4-5

Galactic radiation field

Slide 4-6

Energy of cosmic ray particles

F(>E): Flux of particles with energies >E

LHC-limit Slide 4-7

MAGIC Cherenkov-Telescope (ETH participation)

Slide 4-8

Elemental abundances of the cosmic ray particles

Slide 4-9

[OII] and [SII] density diagnositics

from Osterbrock (1974)

Slide 4-10

[OIII] temperature diagnostics

from Osterbrock (1989)

Slide 4-11

Spectrum of the Orion nebula

f From www.astrosurf.com Slide 4-12

HI transitions

Slide 4-13

He I transitions

Slide 4-14

ζ Oph, HI Lyα absoption

The interstellar absorptions in the FUV were studied around 1973 with the Copernicus stellite. A detailed study of ζ Oph, the brightest O-star, was used for a line survey (Morton 1974, ApJ 197, 85). This part of the spectrum shows: the damped Lyα 1215A line, three NI lines at 1200A, SII lines at 1250A and many other weak lines. The broad, shallow absorptions arund 1237A are from the star.

Slide 4-15

ζ Oph, FUV spectrum

c

Slide 4-16

Spectrum from 1000A to 1200A: There are many very strong absorptions from Molecular hydrogen H2, many narrow atomic lines, and broad, shallow stellar lines.

ζ Oph, H2 absoption

Small spectral region with strong absorptions from H2

Slide 4-17

Interstellar absorption

Effective absorption cross section for interstellar gas (from M. Longair 2011, High energy astrophysics)

Slide 4-18

Bremsstrahlung

Emission by an accelerated charge (from M. Longair 2011, High energy astrophysics)

Slide 4-19

CO cooling lines in M82

From Panuzzo et al. 2010, A&A 518, L37 Slide 4-20

Line spectra of spiral galaxies

from Kennicutt, 1992, ApJS 79, 255 Slide 4-21

X-ray spectrum of the SN shell Cas A

from NASA/Chandra supernova catalog (http://hea-www.cfa.harvard.edu/ChandraSNR/sample_spectrum.html)

Slide 4-22

Supernova shells

Crab nebula Tarantula nebula LMC Slide 4-23

Collisional IonizationPhotonionization-structure for spherical nebulaeInterstellar polarizationDust in the IR-galaxy M82Magnetic fields in M51Galactic radiation fieldEnergy of cosmic ray particlesMAGIC Cherenkov-Telescope (ETH participation)Elemental abundances of the cosmic ray particles[OII] and [SII] density diagnositics[OIII] temperature diagnosticsSpectrum of the Orion nebulaHI transitionsHe I transitionsζ Oph, HI Lyα absoptionFoliennummer 16Foliennummer 17Interstellar absorptionBremsstrahlungCO cooling lines in M82Line spectra of spiral galaxiesX-ray spectrum of the SN shell Cas ASupernova shells