Radioactive elements in metal deficient stars
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Transcript of Radioactive elements in metal deficient stars
Slide 1
Radioactive elements in metal deficient stars
Volodymyr Yushchenko
Astronomical observatory, Odessa National University,
Ukraine
Collaborators:
Vira Gopka Odessa, UkraineAlexander Yushchenko, Seoul,
KoreaAngelina Shavrina, Kiev, Ukraine Sergey Andrievsky, Odessa,
UkraineValery Kovtyukh, Odessa, UkraineSvetlana Vasileva, Odessa,
Ukraine, Yakiv Pavlenko, Kiev, UkrainePapakaev Rittipruk, Seoul,
KoreaYoung-Woon Kang, Seoul, Korea
Three metal poor stars:
PMMR 144 V=12.8 SMC red supergiant
RM_1 -667 V=13.1 LMC red supergiant
HD47536 V=5.2 Galaxy halo or intermediate population star, the
host of 2 planets
For these three stars we will present:
Chemical composition 2) Thorium lines
3) Approximation of abundance pattern by scaled Solar system r-process distribution
The possibility of age determination for these stars will be discussed.
PMMR 144 SMC
Spectra were obtained at 3.6 meter ESO telescope (La Silla, Chile)
Observed by Hill, V. S/N is near 100 Resolution R=20000 and
30000
PMMR 144
Spectral interval 5790 - 6835 Effective temperature Teff = 4100 K
log g = -0.7 Vmicro = 4 km/s The atmosphere model was calculated by
R. Luck
PMMR 144, 3 thorium lines
5989.045 6044.433 6619.943
PMMR 144 5989.045
PMMR 144, et al. 6044.433
Comparison of observed abundances with scaled Solar system
r-process distribution
0.25dex
RM_1-667 LMC
Spectra were obtained at 3.6 meter ESO telescope (La Silla,
Chile)Observed by Hill, V.S/N is near 100Resolution R=20000 and
30000
RM_1-667
Spectral interval 5900 - 6700 Effective temperature Teff = 3750
K log g = -1.5 Vmicro = 2.4 km/s The atmosphere model was
calculated by Ya. Pavlenko
Open circles model atmospheres methodFilled circles - spectrum
synthesis method
RM_1-667, 2 thorium lines
6044.433 6112.837
RM_1-667 6044.433
RM_1-667 6112.837
Comparison of observed abundances with scaled Solar system
r-process distribution
HD 47536 Galaxy
Spectra were obtained at 1.5 meter CTIO telescope (Chile)Observed
by Rittipruk, P.S/N is near 100Resolution R=30000
HD 47536
Spectral interval 4105 - 8170 Effective temperature Teff = 4400
K log g = +1.8 Vmicro = 1.5 km/s Castelli & Kurucz (2003)
atmosphere model was used
HD 47536, 1 thorium line
5989.045
HD 47536 5989.045
Comparison of observed abundances with scaled Solar system
r-process distribution
How to find the age ?
The necessary conditions to determine the reliable age are:
1) the information about the initial abundance ratio, usually it
is taken from the standard cosmology; that is why it is necessary
to suppose the validity of this theory; 2) the universality of
r-process, more exactly it is the hypothesis that the abundance
ratios in the products of different supernova explosions are equal;
3) the changes of abundance ratios are mainly due to natural
radioactive decay; the influence of other factors should be
neglected or estimated.
1) Initial abundance ratio
We will not discuss this problem here
2) The universality of r-process
One of the latest investigations of possible nonuniversality of
r-process was made by Ren, J., Chriestlib, N., & Zhao, G. 2012,
A&A, 537, A118. Result: the thorium abundances span a wide
range of about 4.0 dex, and scatter exists in the distribution of
log (Th/Eu) ratios for lower metallicity stars, supporting previous
studies suggesting the r-process is not universal.
3) The changes of abundance ratios are mainly due to natural
radioactive decay
It seems to be not doubted before. The abundance patterns of PMMR
144, RM_1-667, and HD47536 allow us to discuss this
hypothesis.
What are the possible ways to change the abundance ratios in
stellar photospheres ?
1) Natural radioactive decay2) Nuclear reactions in the star3)
Radiative diffusion in hot stars4) Convection in cool stars5)
Accretion of matter from outer space6)
Let us discuss the fifth case
Accretion of matter from outer space
1) The accretion of interstellar gas (Greenstein 1949, Bohm-Vitense
2006) 2) The mass transfer from binary companion (Fowler et al.,
1965, Proffitt & Michaud 1989) 3) The accretion of rocky
material, asteroids & planets (Drobyshevski 1975, Cowley 1977)
4) The dust-gas separation mechanism (Venn & Lambert 1990,
2008) 5) The accretion of accelerated particles (Goriely 2007)
6)
Let us discuss the first case only
Greenstein 1949, ApJ, 109, 121
Yushchenko A. et al. 2013, AJ, in press
Charge-exchange reactions:High energy protons or helium ions from
interstellar environment collide the resonant atoms (the atoms with
second ionization potentials close to 13.6 & 24.6 eV) in
stellar atmosphere and steal an electron from them. The resonance
energies are the ionization potentials of hydrogen and helium (13.6
& 24.6 eV). The newly ionized atoms fly away at high
velocities. The direction of this fly coincide with the movement of
the ionizing particle. That is why part of the ionized atoms can
leave the star, producing the deficiency of corresponding chemical
element.
PupTeff = 6890 Klog g = 3.28
radiativeatmosphere
Am star, prototype of one of the subgroups of Scuti type
variables
2013, Kang Y.-W, Yushchenko A. et al. AJ, 145, 167
LX Per eclipsing binary star, RS Canum Venoticorum type - strong
circumstellar envelope, gaseous streams, strong accretion in the
system, the source of X-rays Teff (A) = 6225 K, log g (A) = 3.92
Teff (B) = 5225 K, log g (B) = 4.42 The components of LX Per have
convective atmospheres with strong accretion.
2013, Kang Y.-W, Yushchenko A. et al. AJ, 145, 167
Emissions of calcium in the atmosphere of LX Per B
The charge-exchange reactions change the abundances in the
atmospheres of components of LX Per faster than the convection
motions return the chemical composition to solar one.
PMMR 144
Most of the elements with second ionization potentials close to
13.6 eV exhibit lower abundances than the other elements.
It can be the sign of charge-exchange reactions in the
atmosphere of PMMR 144 It can be the result of higher density of
interstellar medium in SMC
RM_1-667
The deficiency of elements with second ionization potentials close
to 13.6 eV can be a sign of accretion
Observed and modeled line in the spectrum of RM_1-667.
The emission component in the observed H profile is fitted with the
temperature inversion in the upper layers of stellar
atmosphere.
The emission also can be a sign of higher density of
interstellar medium. It supports the possibility of charge-exchange
reactions in this star.
HD 47536, the host of 2 planets
The mass of the first planet is > 5 mass of Jupiter, the orbital
period is 430 days, the closest distance between the planet and the
host star can be as small as 1.3 astronomical units or 13 radiuses
of the host star. The possibility of accretion is higher in
planetary system.The relative underabundances of elements with
second ionization potentials close to 13.6 eV can be sign of
accretion (charge-exchange reactions).
CONCLUSION The accretion phenomena in the atmospheres of PMMR 144, RM_1-667, and HD47536 change the surface abundances.
For these stars it is impossible to suppose that the changes of abundance ratios are mainly due to natural radioactive decay.
The attempts to estimate the age of these stars using Th/Eu ratios will lead to wrong results.
It is necessary to discuss the possibility of accretion events even for the oldest stars, as these stars crossed the plane of Galaxy and their surface abundances have been influenced by accretion of interstellar gas.
Thank for yourattention!
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