●Jacco Vink●Utrecht University

High Energy Astrophysics:

A View on Chemical Enrichment,

Outflows &

Particle Acceleration

(Feedback at work)

Jacco Vink, NOVA Science Day, Jan 7 2010: Chemical Enrichment, Outflows, & Particle Acceleration

High Energy Astrophysics

2

•HEA aims at understanding the extreme Universe:•The hottest temperatures•Extreme conditions (Neutron stars, Black holes, GRBs)•Most massive structures (clusters, WHIM)•The highest particle energies (Cosmic Rays: up to 1020 eV)

Jacco Vink, NOVA Science Day, Jan 7 2010: Chemical Enrichment, Outflows, & Particle Acceleration

High Energy Astrophysics

2

•HEA aims at understanding the extreme Universe:•The hottest temperatures•Extreme conditions (Neutron stars, Black holes, GRBs)•Most massive structures (clusters, WHIM)•The highest particle energies (Cosmic Rays: up to 1020 eV)

•Last decade has been very successful:X-rays: Chandra (0.5” res.), XMM (throughput), XTE (timing)γ-rays: Integral (low E γ), HESS, MAGIC, Fermi,.. (high E γ imaging)Cosmic ray “telescopes”: Auger (1019-1020EV: directions)

Jacco Vink, NOVA Science Day, Jan 7 2010: Chemical Enrichment, Outflows, & Particle Acceleration

High Energy Astrophysics

2

•HEA aims at understanding the extreme Universe:•The hottest temperatures•Extreme conditions (Neutron stars, Black holes, GRBs)•Most massive structures (clusters, WHIM)•The highest particle energies (Cosmic Rays: up to 1020 eV)

•Last decade has been very successful:X-rays: Chandra (0.5” res.), XMM (throughput), XTE (timing)γ-rays: Integral (low E γ), HESS, MAGIC, Fermi,.. (high E γ imaging)Cosmic ray “telescopes”: Auger (1019-1020EV: directions)

Jacco Vink, NOVA Science Day, Jan 7 2010: Chemical Enrichment, Outflows, & Particle Acceleration

Thermal plasmas & Chemical Enrichtment

3

●X-ray spectroscopy: probe all alpha- & Fe-group elements●Constrain explosion properties of supernovae:

•Type Ia SNRs: constraints on progenitors•Core collapse: asymmetries, explosion not understood

•Clusters: contain integrated SN yields, cooling vs AGN feedback•WHIM: enriched (?), 105-106K intergalactic medium (40% of baryons)•AGN: outflows →enrich and energize gal/intergal. medium (feedback)

●Chandra ●Astro-H ●IXO

●black

Jacco Vink, NOVA Science Day, Jan 7 2010: Chemical Enrichment, Outflows, & Particle Acceleration

Thermal plasmas & Chemical Enrichtment

3

●X-ray spectroscopy: probe all alpha- & Fe-group elements●Constrain explosion properties of supernovae:

•Type Ia SNRs: constraints on progenitors•Core collapse: asymmetries, explosion not understood

•Clusters: contain integrated SN yields, cooling vs AGN feedback•WHIM: enriched (?), 105-106K intergalactic medium (40% of baryons)•AGN: outflows →enrich and energize gal/intergal. medium (feedback)

●Now: Chandra, XMM, Suzaku: up to 2015 → imaging, med. res. spectr.●Future: ASTRO-H (300m2,2014), IXO (3m2,>2020) →hi.res. spectroscopy (E/ΔE~1200)/imaging

●Chandra ●Astro-H ●IXO

●black

Jacco Vink, NOVA Science Day, Jan 7 2010: Chemical Enrichment, Outflows, & Particle Acceleration

The non-thermal Universe

4

●The non-thermal universe: the universe out of equilibrium●Cosmic-rays/particle acceleration:

-109-1015 eV: SN remnants? many smoking guns, no 100% proof-1018-1020 eV: many uncertainties, candidates: AGN, clusters, GRBs?

●Importance: 10% of SN energy to CRs, uGal=1 eV/cm3: -comparable to other forms of energy (radiation/B-field/thermal)!

Jacco Vink, NOVA Science Day, Jan 7 2010: Chemical Enrichment, Outflows, & Particle Acceleration

The non-thermal Universe

4

●The non-thermal universe: the universe out of equilibrium●Cosmic-rays/particle acceleration:

-109-1015 eV: SN remnants? many smoking guns, no 100% proof-1018-1020 eV: many uncertainties, candidates: AGN, clusters, GRBs?

●Importance: 10% of SN energy to CRs, uGal=1 eV/cm3: -comparable to other forms of energy (radiation/B-field/thermal)!

●Many links to low energy astrophysics: -Thermal astronomy: energy budget (e.g. Helder+, Science ʼ09)-Source of energy: ionization, magnetic field amplification-Tracer: - diffuse radio synchrotron: CR electrons →B-field

-TeV astronomy: light up molecular clouds (HESS)●Broad: synchr. (107-1018Hz), IC (1018-1028Hz), pions (1024-1028Hz),CRs

Jacco Vink, NOVA Science Day, Jan 7 2010: Chemical Enrichment, Outflows, & Particle Acceleration

The non-thermal Universe

4

●The non-thermal universe: the universe out of equilibrium●Cosmic-rays/particle acceleration:

-109-1015 eV: SN remnants? many smoking guns, no 100% proof-1018-1020 eV: many uncertainties, candidates: AGN, clusters, GRBs?

●Importance: 10% of SN energy to CRs, uGal=1 eV/cm3: -comparable to other forms of energy (radiation/B-field/thermal)!

●Now: HESS, MAGIC, VERITAS (TeV), Fermi (GeV), Auger (CRs)

●Future: Cherenkov Telescope Array (EU), AEGIS (US), Auger North KM3Net

●Many links to low energy astrophysics: -Thermal astronomy: energy budget (e.g. Helder+, Science ʼ09)-Source of energy: ionization, magnetic field amplification-Tracer: - diffuse radio synchrotron: CR electrons →B-field

-TeV astronomy: light up molecular clouds (HESS)●Broad: synchr. (107-1018Hz), IC (1018-1028Hz), pions (1024-1028Hz),CRs