#63: A supernova-driven wind model for high-z galaxiesMori, Yajima & Umemura (Univ. of Tsukuba)

log10XHI

-8

-4

0

z=7.0 z=5.8

z=5.0 z=3.7

RT cal.

LAEs

LBGs

Ionization structure

Model galaxy(Mori&Umemura 2006)

LAE phase LBG phase

We have suggested that Lyα emitters can be identified with primordial galaxies catched in a supernova-dominated phase.

After 500 Myr, the metal abundance reaches already the level of solar abundance.

Solving three dimensional radiation transfer (RT) equation, LAEs and LBGs have a large escape fraction of the ionizing photon.

Simulated Observed Lyman alpha emission image

Three-dimensional Hydrodynamic Model of Lyman-alpha Emitters (LAE)

Gamow-Teller Strengths in Proton Rich Exotic Nuclei

Deduced from Mirror Transitions ID-68ID-68

bottlenecks & waiting points in nucleosynthesis

bottlenecks – reaction flow proceeds almost totally through one reaction

both can CHANGE energy generation & element synthesis

you can use our online system to perform customized searches for bottlenecks and waiting points in your simulations

waiting points – flow to higher masses interrupted by long beta decay

in XRB and novaein XRB and novaeSmith, Sunayama, Hix, Lingerfelt, NesarajaSmith, Sunayama, Hix, Lingerfelt, Nesaraja

also… sensitivity studies [vary input rates] are now automated

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nuclearmasses.orgrepresents a tremendous new capability in research with exotic beams researchers from around the world can benefit from RIBF data 

• makes it easy to access, compare, analyze,

visualize mass data sets …• upload and share your own mass models,

measurements …• new features: additional quantities

like S2n plots, dVpn …

Smith, Lingerfelt, Koura, Nesaraja, Kondev ORNL JAEA ANL

• nuclear masses: important, active research area,

but poor distribution, visualization

measurements

GSI ESR

theoretical models

Skyrme force (Vautherin & Brink)

• software solution: nuclearmasses.org -- a

free online system

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recoil separator for capture measurements at FRIB

Focal plane

where: Facility for Rare Isotope Beams [FRIB] – to be built at Michigan State University

use: directly measure (p,) reactions on radioactive nuclei in novae & X-ray bursts

SECAR status: funded 6.2 M$, collaboration formed, design work underway

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The 10th. International Symposium on Origin of Matter and Evolution of the Galaxies (OMEG10) 08-10 March 2010

Annihilation Lines at 255.5 keV and at 511 keV in the Radiation Spectrum from the Pulsar SurfaceV.M. Kontorovich, O.M. Ulyanov, A.B. Flanchik

Institute of Radio Astronomy of NAS of Ukraine; 4 Chervonoprapona str., Kharkov 61002, Ukraine, (oulyanov@kharkov.ua)

Fig. 1Formation of the annihilation line 255.5 keV due to annihilation of

positrons from the vacuum gap with electrons of the pulsar polar cap surface.

Fig. 4Forming of the annihilation lines at 255.5 keV (near the surface) and at 511

keV due to annihilation of the relativistic positrons in the substance and evolution in the radiation pattern of annihilation in proportion to decelerating positrons.

The angular distribution of the differential cross section of the two-photon annihilation in the electron rest frame.

The scheme of the observation of lines at 255.5 keV and at 511 keV for the annihilation

of the rapid positrons.

The Detectors 1 - 6 are intended for registering of the emission line at 511 keV from the annihilation of rapid positrons, moreover by detector 4 must be recorded the annihilation line at 255.5 keV (hν≈ mec2/2).

Poster #79

The 10th. International Symposium on Origin of Matter and Evolution of the Galaxies (OMEG10) 08-10 March 2010

Interaction of the Ultra Relativistic Pulsar Plasma with the Upper Atmosphere of the Star - Companion O.M. Ulyanov

Institute of Radio Astronomy of NAS of Ukraine; 4 Chervonoprapona str., Kharkov 61002, Ukraine, (oulyanov@kharkov.ua)

Fig. 1Comparison of different types of the losses of the

electron/positron of that moving in the photosphere of the HD 21699. Figure gives the relative (to the speed of all ionizing losses) values of the speeds of the synchrotron, bremsstrahlung and Compton losses of electron. The relative speeds of the synchrotron losses for B

┴ = 1 kG,

B┴

= 5 kG, B┴

= 10 kG respectively and the relative speed of the bremsstrahlung losses for the weakly ionized plasma (thick solid line).

Fig. 2The life time of the fast electrons/positrons in the

chromosphere of the star. The upper curve corresponds to the life time of electron in the Sun chromosphere. The transit time of the photon through the solar chromosphere is approximately equal to 5.6 ms (lower horizontal line). Middle and lower curves correspond to the life time of electrons in the chromosphere of the star HD 21699. The strength of perpendicular component of magnetic field is taken to be equal to B

┴ =1 kG for middle and B

┴ =10 kG for the

lower curve respectively.

Fig. 4An example of the spectra of the

synchrotron radiation, the bremsstrahlung, and the inverse Compton emission for different layers of the upper atmosphere of the star- companion and different conditions.

Fig. 3Comparison of the dimensionless kinetic energy of

primary electrons (X-axis) with the kinetic energy of the electrons that passed through photosphere of the HD21699 (Y-axis). The upper curve corresponds to kinetic energy of the primary electrons (γ'-1) on the top of the convection zone. Further from the left to right curves are located that characterize dimensionless kinetic energy of electron on the border between the photosphere and convection zone for the value of B

┴ = 1 kG, B

┴ = 5 kG and B

┴ = 10

kG.

Poster #78

The 10th. International Symposium on Origin of Matter and Evolution of the Galaxies (OMEG10) 08-10 March 2010

The nature of Magnetic Chemically Peculiar (MCP) stars through the prism of inexplicable factsVira Gopka - Astronomical Observatory, Odessa National University, Odessa, Ukraine; (vera.gopka@mail.ru); Oleg Ulyanov - Institute of Radio Astronomy of NAS of Ukraine, Kharkov;Alexander Yushchenko - ARCSEC, Sejong University, Seoul, Korea ;Angelina Shavrina - Main Astronomical Observatory of NAS of Ukraine, Kiev, UkraineSergey Andrievsky - Astronomical Observatory, Odessa National University, Odessa, Ukraine.

Fig. 2The fit of model T

eff=6600 K, lg(g)=4.2 (Shavrina et al.

2003, A&A, 409, 707) to observed UVES Hα profile of HD 101065. In spite of Kochukhov et al. 2002 (ApJ, 578, L75) interpretation of core-wing anomaly we see an emission in blue part of asymmetric Hα core (atmospheric lines are taking into account)

Fig. 1The schematic picture of radio emission of MCP

stars in the model MCP star+NS. According to Drake et all., (1987) “ The radio emission is consistent with gyro synchrotron emission from continuous ejected , mildly relativistic nonternal particle trapped in the magnetosphere”.

Fig. 4The additional heating of the photosphere of MCP star. In fact the additional heating of the part of the star photosphere, which turnover to the pulsar will be uneven. This non homogeneous heating can lead to the appearance of short-period pulsations of the brightness of star, to the fluctuations of the tension of magnetic field, and to the appearance of orbital modulations of observed MCP star parameters. Finally, the consequence of interaction pulsar -MCP star in the close binary system can be the reason of the appearance of short-lived isotopes in the upper atmosphere of star.

Fig. 3 The picture explains the anticorellation of radio

emission and magnetic field and the map of radio emission near the MCP star relative us. Left part of the figure is taken from Drake et al., (1987) .

Poster #80

Conclusion

The present model can explain a lot of the inexplicable facts which are known from the recent observations of MCP stars.