Nuclear gamma-rays from hot accretion flows

Felix Aharonian DIAS/Dublin and MPIK/Heidelberg

Nucleosynthesis for a Life: A symposium in honour of R. Diehl

MPE, Munich, Feb 8, 2019

prompt de-excitation gamma-ray lines:

unique messengers of information about sub-relativistic Nonthermal Universe

initiated by suprathermal CRs - energy range 1 to 100 MeV implications: solar flares (main energy release)

star forming regions (ionisation, chemistry) SNRs - problem of injection

ISM - pressure …………… - realization - so far, not impressive (except for Solar Flares) the status of “de-excitation gamma-ray line” astronomy - same as in the 1970s

- reason - low efficiency of production (10-5 or less) and lack of sensitive MeV detectors

- future - ?? , partly eASTROGAM, …

100 MeV does not necessarily imply “nonthermal”

formation of hot 1010 K to 1012 K plasmas?

due to accretion on neutron stars and black holes

termination of sub-relativistic shocks: v ~ 0.03-0.3 c

typically two-temperature plasmas with Ti >> Te

de-excitation lines - the best carriers of information about two-temperature plasmas!

radiation efficiency? - somewhat better than in non thermal scenarios!

my “entrance” to Astrophysics started with prompt gamma-ray lines

motivation “rich” physics where I could use my knowledge in nuclear physics

but also

disappointment low radiation efficiency + low performance of MeV detectors

=> shift of interest to (very) higher energies

F.A. Aharonian and R.A. Sunyaev

35 years old almost unnoticed (only 48 citations!) paper

Science with e-ASTROGAMJournal of High Energy Astrophysics, Volume 19, p. 1-106

New interest to the topic:

Gamma-ray line formation in hot plasmas - result of operation of large amount of excitation and spallation reactions in 1-100 MeV region

=> detailed nuclear reaction codes are required now available (e.g. TALYS) !

New detectors: eASTROMAG

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very good resolution for broad γ-ray lines!

adequate performance for meaningful probes

Phys. Rev D, 2019, accepted

A&A, 2019, accepted

Emissivity of radiation at three different epochs: 10-5 s, 10-2 s, 1 sec

Evolution of Chemical composition

kTi=50 MeV, kTe=100 keV; n=1017 cm-3; solar composition

kTe=100 keV; n=1017 cm-3; solar composition

kTi=30 MeV

kTi=100 MeV

Evolution of Chemical composition Emissivity of radiation at 10-5 s

chemical evolution with radius r=R/Rs luminosity

principal parameters:

viscosity α

ΒΗ mass m=Μ/Μo =10

accretion rate

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gas pressure/total pressure β;

adiabatic index γ;

electron heating/total heating δ;

advection parameter f

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10-3 initial solar composition; α=0.1; f=0.86

π0 Maxwellsharp cutoff at 4kTpower-law after 4kT

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0.0153 α=0.3

Solarcomposition

In the ADAF regime, total gamma-ray line luminosity varies between 3x1031 - 1033 erg/s

in principle, can achieve 1034 erg/s for the “heavy initial composition

π0 decay gamma-ray luminosities between 1034 - 3 1035 erg/s

sensitivity eASTROGAM: at MeV energies 1033 (d/1kpc)2 erg/s around 100 MeV 1032 (d/1kpc)2 erg/s

detection of gamma-ray lines? yes, if we are lucky

detection of π0 decay gamma-rays? yes

but why we did not detect so far with Fermi LAT?