Enrichment of r-process elements in nearby dsph galaxies, the Milky way, and globular cluster(s)
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1 Enrichment of r-process elements in nearby dsph galaxies, the Milky way, and globular cluster(s) Toshikazu Shigeyama (U. Tokyo) Based on Tsujimoto & TS 2014
2 Kilonova Afterglow of GRB130603B at day 9! Berger+ 13, Tanvir+ 13! NIR detection! Absolute Magnitude H i r g Magellan/Gemini Kilonova (M =0.1, v =0.2c) ej ej Kilonova (M =0.01, v =0.2c) ej ej Afterglow (F t 2.6 ) ν HST SN2006aj no detection of optical band Rest Frame Time (d)
3 Kilonova Afterglow of GRB130603B at day 9! Berger+ 13, Tanvir+ 13! NIR detection! no detection of optical band
4 Kilonova Time since GRB B (d) X-ray Afterglow of GRB130603B at day 9! Berger+ 13, Tanvir+ 13! NIR detection! AB magnitude F606W F160W X-ray flux (erg s 1 cm 2 ) 27 no detection of optical band Time since GRB B (s) 10 6
5 Summary of Kilonova short GRB is a result of neutron star merger (NSM)! 1.ejects r-process rich matter! 2.Mass~0.01 M! 3.speeds~>0.1c! 1 & 2 motivate us to revisit NSM as a major production site of r- process elements
6 Transfer properties The speed of ejecta = c (γ= )! Stopping length!! l S ~ 400 kpc v 0.2c 2 A 153 Z eff 63 2 n 1 Fe (from SN): ls ~0.1/n kpc! Most of ejecta escape from a galaxy?
7 Effects of magnetic fields If B~1 #G! rg ~ cm<<size of a galaxy! r-process elements propagate along B fields (kinetic pressure<<magnetic pressure)! Structure of B decides the dissipation of kinetic energy of r-process elements! turbulent B may stop r-process elements through ionizations! r-process elements pervade the entire proto-galactic cloud (with some leakage)
8 Transfer properties The speed of ejecta = c (γ= )! Energy per nucleon =m u c 2 (γ-1)= MeV/A! If 0.3c, then spallation occurs before traveling through the stopping length! If 0.1c, then below the threshold energy
9 r-process elements in extremely metal-poor stars(emp stars) in the Milky Way Large dispersion in [Eu/Fe]! Supernova supplies ~0.1 M Fe! SNR sweeps and mixes ISM of mass ~10 5 M : [Fe/H]~-3! Assume that stars are formed in the swept up gas From SAGA (Suda+ 08)
10 r-process elements in EMP stars in ~7/n Myr after a NS merger! r-process elements could be uniformly distributed! concentration of r-process elements is determined by the cloud mass! How much fraction is trapped inside the cloud is unknown (Assume 100% here)! High(Low) [r-process/fe] low (high) cloud mass! EMP stars were formed in gas swept up by individual SNe! Fe abundance is determined by the SN+ISM
11 Chemical evolution model Fe is mixed in a shell swept up by a SNR (the mass~10 5 M )! r-process elements diffuse over the entire proto-galactic cloud.! NSM rate: Eu/H-Fe/H relation in massive dsphs! Chemical evolution in clouds with different masses! Blue: ~10 9 M! Red: M! [Eu/Fe] Green: 5 105, M (with a few NSM events) [Fe/H]
12 Chemical evolution model Fe is mixed in a shell swept up by a SNR (the mass~10 5 M )! Cannot rule out NSM as the origin of r-process elements. r-process elements diffuse over the entire proto-galactic cloud.! NSM rate: Eu/H-Fe/H relation in massive dsphs! Chemical evolution in clouds with different masses! Blue: ~10 9 M! Red: M! [Eu/Fe] Green: 5 105, M (with a few NSM events) [Fe/H]
13 A few comments on faint dsphs
14 r-process elements in dsphs Ultra Faint dsphs no evolution or sudden increase of Eu in small mass dsphs! Eu/H independent of the masses of dsphs! dsph masses are small! Suppose NSM supplies Eu! [Eu/H] Draco faint dsph Sculptor Carina very few NSM events! a small fraction of Eu were trapped (High velocity!) -2.5 Fulbright Eu H X Eu M ej X H M cl [Fe/H] R l S X M Eu ej R 2 X H
15 r-process elements in dsphs Suppose SNe supply Eu in Draco! Ultra Faint dsphs [Fe/H]=-2.3 requires ~500 SNe! faint dsph The mass of the protogalactic cloud~10 7 M (L~ L )! [Eu/H] Draco Sculptor Carina No enrichment in Eu/H by the subsequent 2500 SNe! -2.5 Fulbright [Fe/H] disfavors SNe as a source of r-process elements
16 r-process elements in globular cluster b) M15(Otsuki+ 2011, Roederer 2013, Worley+ 2013)! massive and metal-poor ([Fe/H]~-2.3)! hosts some double pulsars! [La/H] [Eu/H] variation in [Eu/H], [La/H], and [Ba/ H]! Worley no significant variation in [Fe/H]
17 Stellar surface polluted with NSM ejecta? Red-giants with r-process excess! Possible scenario! Number 8 6 First star formation event! 4 all supernovae went off! all the gas component removed! less massive stars evolved to AGB and supplied gas! [Eu/H] NSM enriched the gas with r-process elements! still less massive dwarfs have accreted the r-process rich gas
18 some dwarfs become extremely r-process rich! the dwarfs evolved to red-giants to be observed! The distribution with respect to r-process elements becomes bimodal.
19 Summary Milky way halo! mixing of r-process elements different from heavy elements ejected by SNe! Eu/Fe determined by proto-galactic cloud mass! Milky way halo composed of stars formed in various proto-clouds with different masses
20 dsph galaxies! Discrete increases in Eu/H! Common plateau of Eu/H with increasing Fe/H prefers NSM but needs early occurrence(~10 Myr)! Globular cluster M15! Stars with different Eu/H ratios with the same Fe/H! apparently rule out SNe as the source of r-process! SNe that eject r-process elements always eject Fe
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