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SUMMARY:Scalar-isovector channel of the nucleon-nucleon interaction in the
RMF theory and massive compact stars
DTSTART;VALUE=DATE-TIME:20151003T130000Z
DTEND;VALUE=DATE-TIME:20151003T134000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854725@indico.cern.ch
DESCRIPTION:Speakers: Grigor Alaverdyan (Yerevan State University)\nWe dis
cuss the role of scalar-isovector channel of nucleon-nucleon interaction i
n the framework of RMF theory to describe the equation of state of neutro
n star matter. It is shown that taking into account of this channel of int
eraction leads to a more stiff equation of state of hadronic component and
\, consequently\, to an increase in the maximum mass of a compact star. In
fluence of scalar-isovector channel of interaction on the parameters of th
e quark-hadron phase transition is also studied. The integral parameters o
f the hybrid star are compared to each other with and without considering
this type of interaction. The results obtained for the maximum mass of com
pact stars are compared to the values of the mass of recently observed mas
sive neutron stars.\n\nhttps://indico.cern.ch/event/360350/contributions/8
54725/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854725/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Addresses by the YSU Rector\, Dean of Physics Faculty and Organize
rs
DTSTART;VALUE=DATE-TIME:20150930T133000Z
DTEND;VALUE=DATE-TIME:20150930T134000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854734@indico.cern.ch
DESCRIPTION:https://indico.cern.ch/event/360350/contributions/854734/
LOCATION:Physics Department 2nd Floor Conference Room
URL:https://indico.cern.ch/event/360350/contributions/854734/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Noether and Lie symmetries of the field equations and their invari
ant solutions in Hybrid Gravity
DTSTART;VALUE=DATE-TIME:20150930T203000Z
DTEND;VALUE=DATE-TIME:20150930T210000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854737@indico.cern.ch
DESCRIPTION:Speakers: Aneta Wojnar (Univ. of Wroclaw)\nSymmetries play an
important role in physics and\, in particular\, the\nNoether symmetry theo
rem is a useful tool to select models motivated at a\nfundamental level. M
oreover\, the symmetries help to find exact \nsolutions of equations deriv
ed from a Lagrangian. In this work\, we \nconsider the application of poin
t\nsymmetries in the recently proposed hybrid metric-Palatini gravitationa
l\ntheory in order to select the f(R) function and to find analytical\nsol
utions of the field equations and of the Wheeler-DeWitt equation in\nquant
um cosmology.\n\nhttps://indico.cern.ch/event/360350/contributions/854737/
LOCATION: Small Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854737/
END:VEVENT
BEGIN:VEVENT
SUMMARY:From macro to micro: universal properties of neutron stars
DTSTART;VALUE=DATE-TIME:20151001T153000Z
DTEND;VALUE=DATE-TIME:20151001T161000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854747@indico.cern.ch
DESCRIPTION:Speakers: Andrea Maselli (Eberhard Karls University of Tübing
en)\nUniversal I-Love-Q relations connect the moment of inertia\, the tida
l Love numbers \nand the quadrupole moment of a neutron star. Such identit
ies are nearly independent \nfrom the star internal composition\, and ther
efore they represent a valuable tool to test \nits features irrespective o
f the equation of state. \nIn this talk will review the recent progress on
the field. I will explore the \ndomain of validity of I-Love-Q relations\
, and the attempts to provide a comprehensive description of their physica
l origin. Finally\, I will show the prospect to use them \nwith future gra
vitational and electromagnetic observations\, \nto constraint the neutron
star internal composition\, and to derive information on its physical env
ironment.\n\nhttps://indico.cern.ch/event/360350/contributions/854747/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854747/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Stiffening baryonic equation of state with hyperons
DTSTART;VALUE=DATE-TIME:20151002T202000Z
DTEND;VALUE=DATE-TIME:20151002T210000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854753@indico.cern.ch
DESCRIPTION:Speakers: Ghazanfari Mojarrad Mehdi (University of Kashan)\nSt
udy of the structure and properties of neutron stars (NS) has attracted e
ver increasing theoretical and observational efforts during the last few d
ecades [1]. The baryonic equation of state (EOS) is an essential step towa
rds creating an efficient and convenient model\nfor NS structure and compo
sition [2-4]. Recent observations of two solar-mass NS\, lead the EOS of
theoretical models to a more stiff behavior until a value greater\nthan of
this value for the maximum mass of NS is obtained. Due to rapid increase
of the nucleon\nchemical potential with density\, hyperons are expected to
appear.\nWhen strange matter is included in the structure\, the EOS gets
an\ninevitable soft behavior. Having large rest mass of\nhyperons\, reduce
s of the kinetic energy density and lies these\nparticles at lower moment
um states. Therefore the EOS with\nhyperons needs to be stiffer. We can ov
ercome to this softening mechanism\nthrough a generalized interaction to r
each finally the value upper than\n$2M_{\\odot}$ for maximum mass of NS. T
his generalized\ninteraction of Myers and Swiatecki (MS) type [2\,3] with
explicit density and momentum\ndependent strength in phase space is:\n$$\
nV_{12}=-2 \\ G_{B1\,B2} \\ \\rho^{-1}_0 f (\\frac{r_{12}}{a}) \\\n\\{\\fr
ac{1}{2}(1\\mp\\xi)\\alpha-\\frac{1}{2}(1\\mp\\zeta)\\times[\\beta(\\frac{
p_{12}}{p_b})^2\n-\\gamma(\\frac{p_b}{|p_{12}|}) +\\sigma\n(\\frac{2\\bar\
\rho}{\\rho_0})^{{\\frac{2}{3}}}]\\}\nf(\\frac{r_{12}}{a})\n$$\n$$\nV_{12}
=\\frac{1}{4\\pi{a^{3}}}\\frac{exp(-\\frac{r_{12}}{a})}{\\frac{r_{12}}{a}}
\n\\bar{\\rho}^{\\frac{2}{3}}=\\frac{1}{2}(\\rho^{\\frac{2}{3}}_{1}+\\rho^
{\\frac{2}{3}}_{2}).%\\hspace{10.9cm}\n$$\n\nThe interaction between like
and\nunlike particles can be distinguished by $\\textit{l\,u}$ where\n the
minus and plus signs indicate to like and\nunlike particles respectively:
\n\n$$\n\\alpha_{l\,u}=\\frac{1}{2}(1\\mp\\xi)\\alpha \\ \,\\\n\\beta_{l\,
u}=\\frac{\\eta}{2}(1\\mp\\zeta)\\beta \\ \, \\\n\\gamma_{l\,u}=\\frac{1}{
2}(1\\mp\\zeta)\\gamma \\ \, \\\n\\sigma_{l\,u}=\\frac{\\eta}{2}(1\\mp\\ze
ta)\\sigma\,\n$$\n\nwhere $\\eta=1$ as that of MS potential for nucleon-nu
cleon\ninteraction and $\\eta=(\\frac{\\rho_{B}}{\\rho_{0}})^{\\frac{2}{3}
}$\nfor hyperon-baryon interaction.\n According to the available\nhypernuc
lei experimental data\, the $\\Lambda$ hyperon gets the best\nknown adjust
able potential well $U_{\\Lambda}^{(N)}\\simeq-30 (MeV)$\nin normal nuclea
r matter. In contrary to the $\\Lambda-N$\ninteraction\, we can't firmly e
xtract the other potential well\ndepths $U_{i}^{(j)}$ known as potential f
elt by baryon i-th in\nsaturation density of baryonic matter j-th. This be
cause\,\nrelated hypernuclear experimental data are scared and ambiguous.\
nFinally\, we can generally adopt the following values\n$U_{\\Sigma}^{(N)}
\\cong+30 (MeV)$\, $U_{\\Xi}^{(N)}\\cong-18 (MeV)$\nand:\n$$\nU_{\\Xi}^{(\
\Xi)}\\cong U_{\\Sigma}^{(\\Xi)}\\cong\nU_{\\Lambda}^{(\\Xi)}\\cong U_{\\S
igma}^{(\\Sigma)}\\cong\nU_{\\Xi}^{(\\Sigma)}\\cong U_{\\Lambda}^{(\\Sigma
)}\\cong\n2U_{\\Lambda}^{(\\Lambda)}\\cong2U_{\\Xi}^{(\\Lambda)}\\cong\n2U
_{\\Sigma}^{(\\Lambda)}\\cong -10 (MeV).\n$$\nAs a result\, the baryon-bar
yon coupling constants $G_{B1\,B2}$ can\nbe adjusted to the above constrai
n values for potential depths. Our main focus has\nbeen dedicated to stud
y the possibility of how much the baryon-baryon\ninteraction can affect to
the stiffness of the EOS to raise the\nmaximum mass of NS in agreement wi
th the resent observed mass. It\nwas shown that the hyperon formation is v
ery sensitive to the\ninteractions furnished by the baryon-baryon coupling
constants. Within our generalized interactions with hyperon degrees of fr
eedom the maximum mass of NS is in the range\n$1.90\\sim2.09 M_{\\odot}$ f
or different interactions whereas within MS interactions this value is in
the range $1.16\\sim1.26 M_{\\odot}$. Our findings about the stellar matte
r\nproperties with strangeness content show the capability\nand the genera
l applicability of our statistical model.\n\n**References:**\n\n[1] M. Cam
enzind\, Compact Objects in Astrophysics (Springer-Verlag\, Berlin\, Heide
lberg\, 2007).\n\n[2] W. D. Myers\, W.J. Swiatecki\, Nucl. Phys. A 601\, 1
41 (1996).\n\n[3] H.R. Moshfegh\, M. Ghazanfari Mojarrad\, J. Phys. G 15\,
085102 (2011).\n\n[4] H.R. Moshfegh\, M. Ghazanfari Mojarrad\, Eur. Phys.
J. A 49 (2013).\n\nhttps://indico.cern.ch/event/360350/contributions/8547
53/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854753/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Piercing the Vainshtein screen: local constraints on modified grav
ity
DTSTART;VALUE=DATE-TIME:20151002T180000Z
DTEND;VALUE=DATE-TIME:20151002T184000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854767@indico.cern.ch
DESCRIPTION:Speakers: Hermano Velten (Centre de Physique Théorique UMR 73
32)\nBy using observations of the Hulse-Taylor pulsar we constrain the gra
vitational wave (GW) speed\nto the level of $10^{-2}$. We apply this resul
t to scalar-tensor theories that generalize Galileon 4 and\n5 models\, whi
ch display anomalous propagation speed and coupling to matter for GWs. We
argue\nthat this effect survives conventional screening due to the persist
ence of a scalar field gradient inside\nvirialized overdensities\, which e
ffectively “pierce” the Vainshtein screening. In specific branches of\
nsolutions\, our result allows to directly constrain the cosmological coup
lings in the effective field\ntheory of dark energy formalism.\n\nhttps://
indico.cern.ch/event/360350/contributions/854767/
LOCATION: Small Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854767/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Purely phenomenological equation of state for nuclear matter
DTSTART;VALUE=DATE-TIME:20151002T145000Z
DTEND;VALUE=DATE-TIME:20151002T153000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854769@indico.cern.ch
DESCRIPTION:Speakers: Jérôme MARGUERON (Institut de Physique Nucléaire
de Lyon)\nThe nuclear equation of state is still a very challenging issue
for nuclear astrophysics\, determining the masses and radii of neutron sta
rs \nas well as the properties of core-collapse supernovae.\nMany nuclear
modeling\, being more or less phenomenological\, exist but the relation be
tween their parameters and \nthe final astrophysical observation is usuall
y quite complex and requires statistical analysis.\nIn this talk\, we will
present a purely phenomenological equation of state which is able to mimi
c all existing modelings that we have tested.\nIt stands for an unifying m
odel for the nuclear equation of state\, which main advantage is the clear
relation between the empirical parameters of nuclear\nmatter and the para
meters of the model.\nWe first apply this new approach to understand the r
elation between masses and radii of neutron stars and empirical parameters
\nand identify the most determinant ones.\n\nhttps://indico.cern.ch/event/
360350/contributions/854769/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854769/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Universal symmetry energy contribution to the neutron star equatio
n of state
DTSTART;VALUE=DATE-TIME:20150930T195000Z
DTEND;VALUE=DATE-TIME:20150930T203000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854761@indico.cern.ch
DESCRIPTION:Speakers: David Alvarez-Castilio (JINR Dubna)\nWe present syst
ematic investigation of the Universal Symmetry Energy Con- jecture (USEC)
starting from the observation made first in [1] that under con- ditions of
charge neutrality and β−equilibrium the contribution from the asym- me
try energy to the equation of state (EoS) for neutron star matter follows
a universal behaviour unless the direct Urca (DU) process becomes allowed.
It reveals that indeed the USEC holds provided the density dependence of
the sym- metry energy Es(n) follows a behaviour that limits the proton fra
ction x(n) to values below the DU threshold. The absence of DU cooling pro
cesses in typical mass neutron stars appears to be supported by the phenom
enology of neutron star cooling data. Two classes of symmetry energy funct
ions are investigated more in detail to elucidate the USEC. Both of them f
ulfill the constraint from a detailed analysis using isobaric analog state
s (IAS) [2] which revealed that E∗ = Es(n∗) = 26 MeV at a reference de
nsity n∗ = 0.106 fm−3.\nThe first one follows an MDI type ansatz Es(n)
= E∗ · (n/n∗)γ where the IAS constraint limits the admissible value
s of γ to the range 2/3 ≤ γ ≤ 9/10 when also the smaller variations
at its lower limit for n = n0/4 are respected. With this ansatz the USEC i
s not directly apparent.\nThe second one uses a recent parametrization of
the density-dependent cou- plings in the isovector ρ meson channel within
the generalized density functional approach to nuclear matter [3] leading
to a moderate increase of the symmetry energy at supersaturation densitie
s\; gentle enough to fulfill the DU constraint in the whole range of densi
ties relevant for neutron star interiors and thus in perfect agreement wit
h the USEC.\nWe discuss that this behaviour is shared with the APR EoS tha
t respects the tensor force of the NN interaction. Note that recent work o
n short range correlations from the tensor force [4] suggests an MDI type
parametrization with γ = 0.8. While this is apparently in line with the I
AS constraint it would fulfill the USEC only for a sufficiently stiff symm
etric part of the nuclear EoS.\n\nhttps://indico.cern.ch/event/360350/cont
ributions/854761/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854761/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Role of r-modes in evolution of recycled neutron stars
DTSTART;VALUE=DATE-TIME:20151001T181500Z
DTEND;VALUE=DATE-TIME:20151001T185500Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854748@indico.cern.ch
DESCRIPTION:Speakers: Andrey Chugunov (Ioffe Institute)\nObservations of h
ot rapidly rotating neutron stars in\nlow-mass X-ray binaries (LMXBs) prov
ide important\nconstraints on the r-mode instability in neutron stars\n(se
e\, e.g.\, Ref. [1]). Here we discuss additional\nconstraints imposed on t
his instability\, which follow from\nobservations of recycled neutron star
s. Recent Ref. [2] was\ndevoted to the same subject and concluded that ''u
ngapped\ninteracting quark matter is consistent with both the\nobserved ra
dio and x-ray data''. However\, this model leads\nto very high neutrino lu
minosity\, thus high temperatures\nobserved for neutron stars in LMXBs can
hardly be explained\n(deep crustal heating is clearly not enough). We arg
ue that\n*all* the models in which r-mode instability is\nsuppressed by th
e bulk viscosity should face the same\nproblem. Therefore we concentrate o
n our recent model [1]\nwhere r-mode instability is suppressed because of
the\nresonant interaction of oscillation modes at some internal\ntemperatu
res (``resonant temperatures''). Here we\ndemonstrate that this model agre
es with observations of\nmillisecond pulsars and provide observational evi
dences\nthat the coupling parameter for resonant mode interaction\nat low
temperatures should be rather large\, in agreement\nwith theoretical expec
tations [1]. Furthermore\, as shown in\nRef. [3]\, in addition to millisec
ond pulsars\, members of\nthe new class of neutron stars -- hot widows/HO
FNARs -- can\nbe born in LMXBs. Recent observations confirm stability of\n
the surface temperature of the quiescent neutron stars\nwithout power-law
components [4]. This could indicate that\nsome of those stars can\, in fac
t\, belong to hot\nwidows/HOFNARs.\n\nThis study was partially supported b
y RFBR (grants 14-02-00868-a and 14-02-\n31616-mol-a)\, and by RF presiden
t programme (grants MK-506.2014.2 and NSh-294.2014.2).\n\nReferences\n\n[1
] M.E. Gusakov\, A.I. Chugunov\, and E.M. Kantor\, Phys.\nRev. Lett. 112\,
151101 (2014)\; Phys. Rev. D 90\, 063001\n(2014)\n\n[2] M.G. Alford and K
. Schwenzer\, Phys. Rev. Lett. 113\,\n251102 (2014)\n\n[3] A.I. Chugunov\,
E.M. Gusakov\, and M.E. Kantor\, MNRAS\n445\, 385–391 (2014)\n\n[4] A.
Bahramian et al.\, MNRAS 452\, 3475–3488 (2015)\n\nhttps://indico.cern.c
h/event/360350/contributions/854748/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854748/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Nuclear pairing from microscopic forces: singlet channels and high
er-partial waves
DTSTART;VALUE=DATE-TIME:20151002T180000Z
DTEND;VALUE=DATE-TIME:20151002T184000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854771@indico.cern.ch
DESCRIPTION:Speakers: Paolo Finelli (University of Bologna)\nPairing gaps
[1] in isospin-symmetric nuclear matter and neutron matter \nare investiga
ted using the chiral nucleon-nucleon potential at the N$^3$LO order\nin th
e two-body sector [2] and the N$^2$LO order in the three-body sector [2\,3
].\n\nAfter a short introduction to chiral potentials and related techniqu
es (renormalization group approaches [4])\, we present results for the sin
glet channel ($^1S_0$) and higher partial coupled waves ($^3PF_2$\nand $^3
SD_1$) [5]. \nThe role of three-body forces and other many-body correlatio
ns is discussed \nin comparison with available {\\it ab-initio} microscopi
c calculations [1\,6] whenever is possible.\n\nWe will also show **(a)** a
preliminary analysis of the Cooper pair wavefunctions and **(b)** the\nex
tension of our formalism to finite temperature in connection with neutron
star cooling mechanisms.\n\n[1] D.J. Dean and M. Hjorth-Jensen\, Rev. of M
od. Phys. **75** (2003) 607\n\n[2] R. Machleidt and D.. Entem\,\n Phys. R
ept. **503** (2011) 1\n\n[3] J.W. Holt\, N. Kaiser and W. Weise\, Phys. R
ev. C **81** (2010) 024002\n\n[4] S.K. Bogner\, R.J. Furnstahl\, A. Schwen
k\, Prog. Part. Nucl. Phys. **65** (2010) 94\n\n[5] S. Maurizio\, J.W. Hol
t and P. Finelli\, Phys. Rev. C **90** (2014) 044003\n\n[6] S. Gandolfi\,
A.Y. Illarionov\, K.E. Schmidt\, F. Pederiva and S. Fantoni\,\n Phys. Rev
. C **79** (2009) 054005\n\nhttps://indico.cern.ch/event/360350/contributi
ons/854771/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854771/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Pulsars with more exactly measured masses as possible candidates o
f strange stars
DTSTART;VALUE=DATE-TIME:20151003T134000Z
DTEND;VALUE=DATE-TIME:20151003T142000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854731@indico.cern.ch
DESCRIPTION:Speakers: Yuri VARTANYAN (Yerevan State University)\nThe stran
ge quark matter $(SQM)$ has been studied for which the bag model was used.
For considered case\, it is shown that neutron stars with small mass and
configurations consisted of $SQM$ form one family on the curve of dependen
ce of equilibrium superdense star mass on central density of energy $ρ_c$
. The groups of the values of constants for bag model were determined\, wh
ich application results in maximal mass of equilibrium configurations $M_{
max}$\, that are bigger compared with the recently precisely determined m
ass of binary radio pulsar $PSR\\ \\ J0348\\div 0432$ equal to $2.01M_{\\o
dot }$. For each series with $M_{max}>2.01M_{\\odot }$\, for configuratio
ns with masses equal to $M_{max}$\, and 2.01\, 1.97 and 1.44 sun masses\,
which were determined from observations with high precision\, the values o
f radius\, entire number of baryons as well as red sift from the strange s
tar surface depending on $ρ_c$ were calculated. In this case it turns out
that all three pulsars with more accurately measured masses may be possib
le candidates for strange stars.\n\nhttps://indico.cern.ch/event/360350/co
ntributions/854731/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854731/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Unified treatment of sub-saturation stellar matter at zero and fin
ite temperature
DTSTART;VALUE=DATE-TIME:20151001T134000Z
DTEND;VALUE=DATE-TIME:20151001T142000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854750@indico.cern.ch
DESCRIPTION:Speakers: Adriana Raduta (IFIN-HH)\nThe standard variational d
erivation of stellar matter structure in the Wigner-Seitz approximation is
generalized to the finite temperature situation where a wide distribution
of different nuclear species can coexist in the same density and proton f
raction condition\, possibly out of β-equilibrium. The same theoretical f
ormalism is shown to describe on one side the single-nucleus approximation
(SNA)\, currently used in most core collapse supernova simulations\, and
on the other side the nuclear statistical equilibrium (NSE) approach\, rou
tinely employed in r- and p-process explosive nucleosynthesis problems. In
particular we show that in-medium effects have to be accounted for in NSE
to have a theoretical consistency between the zero and finite temperature
modeling. The bulk part of these in-medium effects is analytically calcul
ated and shown to be different from a van der Waals excluded volume term.
This unified formalism allows controlling quantitatively the deviations fr
om the SNA in the different thermodynamic conditions\, as well as having a
NSE model which is reliable at any arbitrarily low value of the temperatu
re\, with potential applications for neutron star cooling and accretion pr
oblems. We present different illustrative results with several mass models
and effective interactions\, showing the importance of accounting for the
nuclear species distribution even at temperatures lower than 1 MeV.\n\nht
tps://indico.cern.ch/event/360350/contributions/854750/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854750/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Atmospheres and radiating surfaces of neutron stars with strong ma
gnetic fields
DTSTART;VALUE=DATE-TIME:20151001T130000Z
DTEND;VALUE=DATE-TIME:20151001T134000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854743@indico.cern.ch
DESCRIPTION:Speakers: Alexander Potekhin (Ioffe Institute\; Pulkovo Observ
atory)\nModern space telescopes have provided a wealth of valuable\ninform
ation on thermal radiation of neutron stars which\,\nwhen properly interpr
eted\, can elucidate the physics of\nsuperdense matter in the interior of
these stars. Strong\nmagnetic fields profoundly change the equation of sta
te and\nradiative opacities in the surface layers of neutron stars\nand th
us affect their thermal spectra. Theory of these\neffects is reviewed in t
he talk\, including the conventional\nmodels of deep (semi-infinite) atmos
pheres\, models of\n"naked" neutron stars with condensed radiative surface
s\, and\n"thin" (finite) atmosphere models\, with examples of\napplication
of the theory to tentative interpretations of\nsome observed neutron-star
thermal spectra.\n\nhttps://indico.cern.ch/event/360350/contributions/854
743/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854743/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A new family of compact objects: Dark Compact Planets
DTSTART;VALUE=DATE-TIME:20151001T185500Z
DTEND;VALUE=DATE-TIME:20151001T193500Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854740@indico.cern.ch
DESCRIPTION:Speakers: Laura Tolos (ICE\, Barcelona)\nA new family of compa
ct objects formed by dark matter admixed with neutron star matter and whit
e dwarf material is investigated [1]. We consider non-self annihilating da
rk matter with an equation-of-state given by an interacting Fermi gas. We
obtain new stable\nsolutions\, dark compact planets. For weakly interactin
g dark matter\, the dark compact planets have Earth-like masses and radii
from few Km to few hundred Km\, whereas they have\nJupiter-like masses and
radii of few hundred Km for the strongly interacting dark matter case. T
he dark compact planets could be formed primordially and accrete white dwa
rf material afterwards. They could be observed as exoplanets with unusuall
y small radii. Furthermore\, we find that the recently observed 2 ${\\rm M
}_{\\odot}$ pulsars set limits on the amount of dark matter inside neutron
stars which is\, at most\, $10^{-6}{\\rm M}_\\odot$.\n\n[1] Laura Tolos a
nd Juergen Schaffner-Bielich\, arXiv:1507.08197 [astro-ph.HE]\n\nhttps://i
ndico.cern.ch/event/360350/contributions/854740/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854740/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Electromagnetic Casimir densities for a cylindrical boundary in de
Sitter spacetime
DTSTART;VALUE=DATE-TIME:20151002T184000Z
DTEND;VALUE=DATE-TIME:20151002T192000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854739@indico.cern.ch
DESCRIPTION:Speakers: Aram Saharian (Yerevan State University)\nQuantum va
cuum effects are investigated for the electromagnetic field\,\ninduced by
a conducting cylindrical shell in background of $(D+1)$\n-dimensional de S
itter spacetime. We assum that the field is prepared in the\nBunch-Davies
vacuum state. A complete set of the electromagnetic field mode\nfunctions
is determined. By using these mode functions\, the vacuum\nexpectation val
ues (VEVs) of the electric field squared is evaluated for\nboth exterior a
nd interior regions. The VEVs are decomposed into the\nboundary-free and b
oundary-induced contributions. The behavior of the latter\nis investigated
in various asymptotic regions of the parameters. For $D=3$\nthe boundary-
induced VEV is related to the corresponding result for a\ncylindrical shel
l in Minkowski spacetime by standard conformal relation.\n\nhttps://indico
.cern.ch/event/360350/contributions/854739/
LOCATION: Small Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854739/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A neutron star on a computer: recent developments
DTSTART;VALUE=DATE-TIME:20150930T142000Z
DTEND;VALUE=DATE-TIME:20150930T150000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854746@indico.cern.ch
DESCRIPTION:Speakers: Jerome Novak (CNRS - Observatoire de Paris)\nRealist
ic global neutron star models require numerical approach. In this talk\, I
shall briefly motivate and recall the general-relativistic framework for
the description of rotating compact stars and show how global observable q
uantities can be computed unambiguously. Then\, I will present some recent
results on the building of more detailed physical models\, including real
istic microphysics\, following three directions. First\, I shall describe
the inclusion of magnetic field and its effects on both\, global equilibri
um and equation of state\, second I will briefly sketch how one can use t
emperature-dependent approach in stationary models\, and finally I will di
scuss superfluid (two-fluid) models in an attempt to model glitch phenomen
a.\n\nhttps://indico.cern.ch/event/360350/contributions/854746/
LOCATION:Phys. Dep.\, YSU 2nd floor Conference Room
URL:https://indico.cern.ch/event/360350/contributions/854746/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Hyperons and Neutron Stars
DTSTART;VALUE=DATE-TIME:20151001T145000Z
DTEND;VALUE=DATE-TIME:20151001T153000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854749@indico.cern.ch
DESCRIPTION:Speakers: Isaac Vidana (University of Coimbra)\nIn this talk I
briefly review some of the effects of hyperons on\nneutron and proto-neut
ron star properties. I revise the problem\nof the strong softening of the
EoS\, and the consequent reduction\nof the maximum mass\, due to the prese
nce of hyperons\, a puzzle\nwhich has become more intriguing due the recen
t measurements of\nthe unusually high masses of the millisecond pulsars\nP
SR J1903+0327 (1.667+/.0.021Msun)\, PSR J1614-2230 (1.97+/-0.04Msun)\nand
PSR J0348+0432 (2.01 +/- 0.04 Msun). I examine also the role of\nhyperons
on the cooling properties of newly born neutron stars and on\nthe so-calle
d r-mode instability.\n\nhttps://indico.cern.ch/event/360350/contributions
/854749/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854749/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Localized oscillating configurations formed by real scalar fields
DTSTART;VALUE=DATE-TIME:20150930T184100Z
DTEND;VALUE=DATE-TIME:20150930T192000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854741@indico.cern.ch
DESCRIPTION:Speakers: Gyula Fodor (Paris Observatory)\nSelf-gravitating re
al scalar fields can form extremely long living localized spherically symm
etric oscillating objects\, which are generally called oscillatons. These
objects are very similar to boson stars\, except that the geometry is not
static\, the metric components oscillate in time. In case of a zero cosmol
ogical constant oscillatons lose energy very slowly by scalar field radiat
ion. However\, in most cases this radiation is negligibly small\, because
the radiation amplitude decreases exponentially when the total mass of the
oscillaton decreases. Since a negative cosmological constant acts as an e
ffective attractive force\, in that case exactly periodic non-radiating os
cillatons exist\, even for massless non-self interacting scalar fields. Nu
merical and analytical results will be presented about the one parameter f
amily of oscillatons emerging from the nodeless linearized solution of the
problem\, both for the zero and negative cosmological constant cases. The
stability range of these configurations was also investigated by applying
a numerical time-evolution code.\n\nhttps://indico.cern.ch/event/360350/c
ontributions/854741/
LOCATION: Small Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854741/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Inhomogeneous chiral symmetry breaking in isospin-asymmetric matte
r
DTSTART;VALUE=DATE-TIME:20150930T184000Z
DTEND;VALUE=DATE-TIME:20150930T192000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854732@indico.cern.ch
DESCRIPTION:Speakers: Daniel Nowakowski (TU Darmstadt)\nWe investigate the
phase structure of strong-interaction matter within a two-flavor Nambu--J
ona-Lasinio model. For degenerate quark flavors it has already been shown
that the appearance of chiral symmetry-breaking phases with spatially modu
lated order-parameters is possible. Since this might have significant cons
equences on the physics of compact stars\, we analyze the emergence of the
se inhomogeneous phases in isospin asymmetric and charge neutral matter by
allowing the order-parameter to be spatially modulated. We find that the
formation of inhomogeneous chiral symmetry-breaking phases is still possib
le with an imbalance in the quark numbers. While enforcing equal quark per
iodicities\, the appearance of such inhomogeneous phases is energetically
disfavored in isospin asymmetric matter. However\, by allowing unequal qua
rk periodicities it is found that the inhomogeneous phase can be stabilize
d against the additional pairing stress.\n\nhttps://indico.cern.ch/event/3
60350/contributions/854732/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854732/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A self-consistent study of magnetic field effects on hybrid stars
DTSTART;VALUE=DATE-TIME:20150930T210000Z
DTEND;VALUE=DATE-TIME:20150930T213000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854763@indico.cern.ch
DESCRIPTION:Speakers: Bruno Franzon (FIAS\, Goethe-University\, Frankfurt
am Main)\nIn this work we study the effects of strong magnetic fields on h
y\nbrid stars by using a full general-\nrelativity approach\, solving the
coupled Maxwell-Einstei\nn equation in a self-consistent way. The\nmagneti
c field is assumed to be axi-symmetric and poloidal. W\ne take into consi
deration the\nanisotropy of the energy-momentum tensor due to the magneti\
nc field\, magnetic field effects on\nequation of state\, the interaction
between matter and the ma\ngnetic field (magnetization)\, and the\nanomalo
us magnetic moment of the hadrons. The equation of st\nate used is an exte
nded hadronic\nand quark SU(3) non-linear realization of the sigma model t
h\nat describes magnetized hybrid stars\ncontaining nucleons\, hyperons an
d quarks. According to our\nresults\, the effects of the magnetization\nan
d the magnetic field on the EoS do not play an important role o\nn global
properties of these stars.\nOn the other hand\, the magnetic field causes
the central density in these objects to be reduced\,\ninducing major chang
es in the populated degrees of freedom a\nnd\, potentially\, converting a
hybrid\nstar into a hadronic star.\n\nhttps://indico.cern.ch/event/360350/
contributions/854763/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854763/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The quantum vacuum and the structure of empty space-time
DTSTART;VALUE=DATE-TIME:20151002T195000Z
DTEND;VALUE=DATE-TIME:20151002T203000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854738@indico.cern.ch
DESCRIPTION:Speakers: Ashot Gevorgyan (Institute for Informatics and Autom
ation Problems\, NAS of Armenia)\nAccording to quantum field theory\, the
vacuum is a space all kinds of\nenergetic particles and oscillating fields
\, which is in a state of\nstatistical equilibrium is characterized by phy
sical parameters and\nstructure. Since the quantum vacuum pervades the ent
ire extent of the\nuniverse then the study of its properties is a topical
problem for deeply\nunderstanding of cosmology and in general for foundati
ons of modern\nphysics. Assuming that the quantum theory of field is possi
ble precisely\nto describe without perturbation methods then the propertie
s of the vacuum\nobviously will be analogous to the properties of an ensem
ble of the\nquantum harmonic oscillators. For the first time we considered
this\nproblem within limits of the stochastic differential equations of\n
Maxwell--Langevin type. In particular assuming that fluctuations of the\nf
ields satisfy to properties of the ``white\nnoise" \, we proved that the\n
Casimir vacuum in an equilibrium is described by the $10$-dimensional\nspa
ce-time\, where $4D$ is the Minkowski space-time\, while $6D$ is the compa
ct\ntopological space with the linear sizes of order $10^{-20}$ cm. It is
shown\nthat in the compact subspace is localized the main part of vacuum e
nergy\,\nwhich can claim the role of dark energy.\n\nhttps://indico.cern.c
h/event/360350/contributions/854738/
LOCATION: Small Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854738/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Compact stars with quark core
DTSTART;VALUE=DATE-TIME:20151002T195000Z
DTEND;VALUE=DATE-TIME:20151002T202000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854726@indico.cern.ch
DESCRIPTION:Speakers: Anahit Harutyunyan (Yerevan State University)\nFor d
ifferent hybrid models of neutron stars with deconfined quark phase in the
core we investigate structural and observable characteristics to compare
them with the measured data of massive pulsars. The observed constraints w
ould allow learning an opportunity for testing equation of state for both
the hadronic and quark matter phases.\n\nhttps://indico.cern.ch/event/3603
50/contributions/854726/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854726/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Structure of hybrid stars with the Field Correlator Method
DTSTART;VALUE=DATE-TIME:20150930T134000Z
DTEND;VALUE=DATE-TIME:20150930T142000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854757@indico.cern.ch
DESCRIPTION:Speakers: Fiorella Burgio (INFN Sezione di Catania)\nI will di
scuss the structure of hybrid stars built with equations of state (EoS) de
rived in the Field Correlator Method (FCM) for quark matter\, and in the B
ruckner-Hartree-Fock (BHF) theory for the hadronic matter\, including hype
rons. I will show that the FCM equation of state can be accurately repres
ented by the “constant speed of sound” (CSS) parameterization\, which
\nassumes a sharp transition to a high-density phase with density-independ
ent speed of sound. A mapping between the FCM and CSS parameters can be pe
rformed\, according to the chosen values of the quark-antiquark potential
$V_1$ and the gluon condensate $G_2$. The observation of a $2M_\\odot$ neu
tron star mass allows FCM equations of state in a restricted subspace of t
he CSS parameters.\n\nhttps://indico.cern.ch/event/360350/contributions/85
4757/
LOCATION:Phys. Dep.\, YSU 2nd floor Conference Room
URL:https://indico.cern.ch/event/360350/contributions/854757/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Towards a unified equation of state for quark/hadron matter
DTSTART;VALUE=DATE-TIME:20150930T152000Z
DTEND;VALUE=DATE-TIME:20150930T160000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854730@indico.cern.ch
DESCRIPTION:Speakers: David Blaschke (University of Wroclaw)\nThe investig
ations exploring the phase boundary between hadronic matter and the quark-
gluon plasma are in the dilemma that a proper theoretical basis is missing
: a unified approach which can describe both phases on the same footing an
d deal properly with the transition between them. We suggest that a cluste
r virial expansion for quark-nuclear matter [1] formulated within the Φ
−derivable approach [2] to many particle systems with strong correlation
s can fill this gap.\nWe define a generic form of Φ−functionals that is
fully equivalent to a selfconsistent cluster virial expansion up to the s
econd virial coefficient for interactions among the clusters. As examples
we consider nuclei in nuclear matter and hadrons in quark matter\, with pa
rticular attention to the case of the deuterons in nuclear matter and meso
ns in\nquark matter. We derive a generalized Beth-Uhlenbeck equation of st
ate for two-particle states in quark matter [3]\, and outline how the quas
iparticle virial expansion is extended to include arbitrary clusters. The
approach is applicable to nonrelativistic potential models of nuclear matt
er as well as to relativistic field theoretic generalizations of models fo
r quark/nuclear matter like the string-flip model [4]. \nIt is particularl
y suited for a description of cluster formation and dissociation in dense
hadronic matter in compact star interiors and in heavy ion collisions such
as planned for FAIR and NICA.\n[1] D. Blaschke\, Cluster virial expansion
for quark and nuclear matter\, arxiv:1502.06279\n[2] G. Baym\, L.P. Kadan
off\, Phys. Rev. 124\, 287 (1961)\; G. Baym\, Phys. Rev. 127\, 1391 (1962)
.\n[3] D. Blaschke et al.\, Generalized Beth-Uhlenbeck approach Ann. Phys.
348\, 228 (2014).\n[4] G. Roepke\, D. Blaschke\, H. Schulz\, Pauli quench
ing effects in a simple string model of quark/nuclear matter\,\nPhys. Rev.
D 34\, 3499 (1985).\n\nhttps://indico.cern.ch/event/360350/contributions/
854730/
LOCATION:Phys. Dep.\, YSU 2nd floor Conference Room
URL:https://indico.cern.ch/event/360350/contributions/854730/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Cosmology with nonminimal kinetic coupling and a Higgs potential
DTSTART;VALUE=DATE-TIME:20150930T160000Z
DTEND;VALUE=DATE-TIME:20150930T163900Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854765@indico.cern.ch
DESCRIPTION:Speakers: S. V. Sushkov (Institute of Physics\, Kazan Federal
University)\nIn this work we continue an investigation of cosmological sce
narios in the theory of gravity\nwith the scalar field possessing a non-mi
nimal kinetic coupling to the curvature\, $\\kappa\\\, G_{\\mu\\nu}\\phi^{
\\mu}\\phi^{\\nu}$\,\n[1-4]. Earlier\, it was shown that the kinetic coupl
ing provides an essentially new inflationary\nmechanism. Namely\, at early
cosmological times the domination of coupling terms in the\nfield equatio
ns guarantees the quasi-De Sitter behavior of the scale factor: $a(t) \\pr
opto e^{H_\\kappa t}$ with \n$H_\\kappa = 1/ \\sqrt{9\\kappa}$. In Ref. [4
] we have studied the role of a power-law potential in models with non-min
imal kinetic coupling. Now\, we consider cosmological dynamics in such the
models with the Higgs-like potential $V (\\phi ) = (\\lambda /4)(\\phi^2
− \\phi^2_0)^2$. Using the dynamical system method\, we analyze all poss
ible asymptotical regimes of the model under investigation. As the most im
portant result\, we have found that\, if the nonminimal coupling parameter
κ is large enough to satisfy $2\\pi G\\kappa \\lambda \\phi^4_0 > 1$\, t
hen the local maximum of the Higgs potential becomes a stable node\, and i
n this case one gets a late-time quasi-De Sitter evolution of the Universe
. The cosmological constant in this epoch is $\\Lambda_\\infty = \n3H_\\in
fty^2 = 2\\pi\\lambda\\phi_0^4$\, and the Higgs potential reaches its loca
l maximum $V (0) = \\lambda\\phi^4_0/4$. Additionally\, using a numerical
analysis\, we construct exact solutions and find initial conditions leadin
g to various cosmological scenarios.\n\nhttps://indico.cern.ch/event/36035
0/contributions/854765/
LOCATION: 2nd floor Conference Room\, Phys. Dep.\, YSU
URL:https://indico.cern.ch/event/360350/contributions/854765/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Late stage of the Universe evolution taking into account the vacuu
m effects
DTSTART;VALUE=DATE-TIME:20151001T185600Z
DTEND;VALUE=DATE-TIME:20151001T193400Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854742@indico.cern.ch
DESCRIPTION:Speakers: Anna Kotanjyan (Yerevan State University)\nThe inves
tigations of quantum vacuum effects indicate that in the phenomenology the
y are responsible for the existence of the cosmological constant $\\Lambda
$\, and besides in the early de Sitter model one has $\\Lambda\\sim H^4$ (
$H$- is the Hubble parameter)\, whereas for the vacuum energy induced by Q
CD condensate at late times $\\Lambda\\sim H$. \n In the present work\,
on the base of the modified Jordan theory\, we consider models of the exp
anding Universe with a cosmological scalar $\\varphi (y)=\\alpha H^{2}$. F
or different values of the coupling constants $\\xi$ the values of the par
ameter $\\alpha$ are obtained corresponding to an accelerated expansion.\n
\nhttps://indico.cern.ch/event/360350/contributions/854742/
LOCATION: Small Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854742/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Magnetic field of strange stars with rotating superfluid core
DTSTART;VALUE=DATE-TIME:20151002T134000Z
DTEND;VALUE=DATE-TIME:20151002T142000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854755@indico.cern.ch
DESCRIPTION:Speakers: David Sedrakian (Yerevan State Unniversity)\, Mekhak
Hayrapetyan (Yerevan State University)\nThe generation of a magnetic fiel
d and its distribution inside a rotating strange star\nare discussed. The
difference between the angular velocities of the superfluid and\nsupercond
ucting quark core and of the normal electron plasma increases because of\n
spin-down of the star and this leads to the generation of a magnetic field
. The magnetic field distribution in a star is found for a stationary valu
e of difference of angular velocities of these components. In all parts of
the star this field is determined entirely by the total magnetic moment M
of the star which can vary from 10^31-10^34 G·cm^3 for some models of co
mpact stars.\n\nhttps://indico.cern.ch/event/360350/contributions/854755/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854755/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A new RMF based quark-nuclear matter EoS
DTSTART;VALUE=DATE-TIME:20150930T203000Z
DTEND;VALUE=DATE-TIME:20150930T210000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854759@indico.cern.ch
DESCRIPTION:Speakers: Niels-Uwe Friedrich Bastian (Wroclaw University)\nTh
e aim of our work is to develop a unified equation of state (EoS) for\nnuc
lear and quark matter for a wide range in temperature\, density and\nisosp
in so that it becomes applicable for heavy ion collisions as well\nas for
the astrophysics of neutron stars\, their mergers and supernova\nexplosio
ns.\nAs a first step we use improved EoS for the hadronic and quark matter
\nphases (with particular focus on phase space occupation effects) and\njo
in them via Maxwell construction.\nThis gives a solid fundament for furthe
r improvements which aim at a\nunified description of the phase transition
on a more fundamental basis\nby a cluster virial expansion\, which should
then allow for predictions\nof the critical line in the three-dimensional
QCD phase diagram.\n\nhttps://indico.cern.ch/event/360350/contributions/8
54759/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854759/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Wakefield generation by radiation beams of millisecond pulsars
DTSTART;VALUE=DATE-TIME:20151003T145000Z
DTEND;VALUE=DATE-TIME:20151003T153000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854770@indico.cern.ch
DESCRIPTION:Speakers: Zaza Osmanov (School of Physics\, Free University of
Tbilisi\, 0183-Tbilisi\, Georgia)\nWe study the generation of wake fields
(WFs) by means of the high energy emission of pulsars. We examine a relat
ively simplified one dimensional model\, considering the Euler equation\,
the continuity equation and the Poisson's equation in a two-component plas
ma. By linearizing the set of equations we estimate the potential differen
ce created by the WFs and analyze the properties of this structure.\n\nhtt
ps://indico.cern.ch/event/360350/contributions/854770/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854770/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Softening of the Nuclear Matter and the Maximum Mass of the Neutro
n Star
DTSTART;VALUE=DATE-TIME:20151002T210000Z
DTEND;VALUE=DATE-TIME:20151002T213000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854724@indico.cern.ch
DESCRIPTION:Speakers: huni Kh Niakian (University of Tehran)\nThe equation
of state (EOS) of the nuclear matter containing nucleons\, leptons\, and
hyperons as relevant degrees of freedom is calculated in the framework of
the free Fermi gas model at zero temperature. The system is supposed to be
an uncharged mixture of mentioned particles which are in beta-equilibrium
. The threshold density of each particle is determined in such matter. We
find that the appearance of each new particle in the system results in sof
tening the EOS. The equilibrium structure of the neutron star described by
discussed EOS is also studied in the present article.\n\nhttps://indico.c
ern.ch/event/360350/contributions/854724/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854724/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Mass-radius relation of white and strange stars
DTSTART;VALUE=DATE-TIME:20151003T153000Z
DTEND;VALUE=DATE-TIME:20151003T161000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854727@indico.cern.ch
DESCRIPTION:Speakers: Gevorg Hajyan (Yerevan State University)\nWhite dwar
fs (WD) and strange dwarfs (SD) are considered. We investigate the mass-ra
dius relations of these stars. Our investigations are carried out for vari
ous chemical compositions of the matter. It is believed that in both of WD
and SD matters the mass number A of atomic nuclei is constant\, and the a
tomic number Z is determined by the beta equilibrium. It is shown that the
larger the collection of the values of A\, the wider region of existence
of SD on the mass-radius plane. Therefore\, the number of candidates to SD
among observed WD is greater than for A = 56. This fact renders WD and SD
hardly distinguished.\n\nhttps://indico.cern.ch/event/360350/contribution
s/854727/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854727/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Short-range correlations in nuclei and compact stars
DTSTART;VALUE=DATE-TIME:20151001T161000Z
DTEND;VALUE=DATE-TIME:20151001T165000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854723@indico.cern.ch
DESCRIPTION:Speakers: Eliezer Piasetzky (School of Physics and Astronomy\,
Tel Aviv University)\nRecent advances in the study of the short-range str
ucture of nuclei indicate that about 25% of nucleons in medium to heavy
nuclei have momentum greater than Fermi momentum (k > kF). These high-mome
ntum nucleons are found to be predominantly short-range correlated proton-
neutron pairs\, created by the short-range tensor interaction. Since these
high momentum nucleons significantly increase the average kinetic energy
on nucleons in symmetric nuclear matter but not in pure-neutron matter\, t
hey should decrease the value of the kinetic part of the nuclear symmetry
energy. In this talk I will review results from recent studies of correl
ations in nuclei and and their potential implications on astronomical obj
ect denser than nuclei.\n\nhttps://indico.cern.ch/event/360350/contributio
ns/854723/
LOCATION:Yerevan\, Armenia
URL:https://indico.cern.ch/event/360350/contributions/854723/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Quantum effects in anti-de Sitter spacetime for electromagnetic va
cuum state
DTSTART;VALUE=DATE-TIME:20150930T195100Z
DTEND;VALUE=DATE-TIME:20150930T203000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854722@indico.cern.ch
DESCRIPTION:Speakers: Anna Kotanjyan (Yerevan State University)\nThe two-p
oint functions of the vector potential and of the field tensor for the ele
ctromagnetic field in background of anti-de Sitter (AdS) spacetime are eva
luated. First we consider the two-point functions in the boundary-free geo
metry and then generalize the results in the presence of a reflecting boun
dary parallel to the AdS horizon. By using the expressions for the two-poi
nt functions of the field tensor\, we investigate the vacuum expectation v
alues of the electric field squared and of the energy-momentum tensor. Sim
ple asymptotic expressions are provided near the AdS boundary and horizon.
\n\nhttps://indico.cern.ch/event/360350/contributions/854722/
LOCATION: Small Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854722/
END:VEVENT
BEGIN:VEVENT
SUMMARY:On the Kerr solution
DTSTART;VALUE=DATE-TIME:20151001T181600Z
DTEND;VALUE=DATE-TIME:20151001T185400Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854744@indico.cern.ch
DESCRIPTION:Speakers: Roland Avagyan (Yerevan State University)\nCalculati
ons are carried out\, on the base of which the limitations are revealed un
der which the general exact solution for the gravitational field\, created
by a uniformly rotating configuration\, is reduced to the Kerr solution.
It is found that in the derivation of the Kerr solution all the multipole
moments are discarded and\, in addition to the integration constant which
define the mass of configuration\, a parameter is introduced which is resp
onsible for the rotation. Already in the first paper by Kerr\, it was note
d that the solution is an example of algebraically special metric of the s
ame class as the known solution NUT. This allowed to reveal that the Kerr
solution is a particular case of the known four-parameter solution which i
s obtained under the assumption of the potential nature of the angular vel
ocity of the worldlines configuration\, forming the used commoving coordin
ate system.\n\nhttps://indico.cern.ch/event/360350/contributions/854744/
LOCATION:Guesthouse Small Hall
URL:https://indico.cern.ch/event/360350/contributions/854744/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Vacuum currents in braneworlds
DTSTART;VALUE=DATE-TIME:20151002T153000Z
DTEND;VALUE=DATE-TIME:20151002T161000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854728@indico.cern.ch
DESCRIPTION:Speakers: Aram Saharian (Yerevan State University)\nVacuum exp
ectation value (VEV) of the current density is investigated for a massive
charged scalar field with arbitrary curvature coupling in the geometry of
a brane on the background of AdS spacetime with partial toral compact dime
nsions. The presence of a gauge field flux\, enclosed by compact dimension
s\, is assumed. On the brane the field obeys Robin boundary condition and
along compact dimensions periodicity conditions with general phases are im
posed. There is a range in the space of the values for the coefficient in
the boundary condition where the Poincare vacuum is unstable. The vacuum c
harge density and the components of the current along non-compact dimensio
ns vanish. The VEV of the current density along compact dimensions is a pe
riodic function of the gauge field flux with the period equal to the flux
quantum. It is decomposed into the boundary-free and brane-induced contrib
utions. Both these contributions vanish on the AdS boundary. The brane-ind
uced contribution vanishes on the horizon and for points near the horizon
the current is dominated by the boundary-free part. Depending on the value
of the Robin coefficient\, the presence of the brane can either increase
or decrease the vacuum currents. Applications are given for a higher-dimen
sional version of the Randall--Sundrum braneworld model.\n\nhttps://indico
.cern.ch/event/360350/contributions/854728/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854728/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Constraint on the internal structure of neutron stars from pulsar
glitches
DTSTART;VALUE=DATE-TIME:20151002T130000Z
DTEND;VALUE=DATE-TIME:20151002T134000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854768@indico.cern.ch
DESCRIPTION:Speakers: Nicolas Chamel (Université Libre de Bruxelles\, Bel
gium)\nPulsars are spinning extremely rapidly with periods ranging from mi
lliseconds to seconds and delays of a few milliseconds per year at most\,
thus providing the most accurate clocks in the Universe. Nevertheless\, su
dden spin up have been detected in some pulsars like the emblematic Vela p
ulsar. These abrupt changes in the pulsar's rotation period have long been
thought to be the manifestation of a neutron superfluid permeating the in
ner crust of neutron stars. However\, the neutron superfluid has been rece
ntly found to be so strongly coupled to the crust that it does not carry e
nough angular momentum to explain the Vela data. We explore to which exten
t pulsar timing observations can be reconciled with the standard glitch th
eory considering the lack of knowledge of dense matter properties.\n\nhttp
s://indico.cern.ch/event/360350/contributions/854768/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854768/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Inflationary evolution of the Universe within the framework of the
modified JBD theory
DTSTART;VALUE=DATE-TIME:20150930T180000Z
DTEND;VALUE=DATE-TIME:20150930T184000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854751@indico.cern.ch
DESCRIPTION:Speakers: Gohar Harutyunyan (Yerevan State University)\nCertai
n conceptual difficulties arising in the construction of the\ncosmological
evolution of the Universe (horizon and "flatness" problems)\, in\nfact\,
do not affect the Standard Model tested by known observations. They\nallow
to determine reasonable initial conditions for classical Cosmology\,\nthe
inflationary process\, which transforms the exponential expansion near\nt
he Planck time to the power-law one.It is significant that while different
\nareas of space\, being on the "distance" $H_{0}^{-1}$ ($H_{0}$ is the\nc
orresponding Hubble parameter) stop to interact\, the "memory" on the\npre
vious connection remains that solves the horizon problem in the\ninflation
ary model. The "flatness" problem is solved in the case where\nduring some
time period the equation of state is given by $p=-\\varepsilon $.\nIn thi
s case\, during $70$ Hubble times "flat" Universe is formed with\naccuracy
$10^{-60}$. Simultaneously the horizon problem is solved. This\nexotic eq
uation of state occurs naturally in all sustainable models. In\nparticular
\, the dynamics of a scalar field\, under very natural assumptions\,\nlead
s to a satisfactory inflationary expansion. In this work\, within the\nfra
mework of various conformal representations of the modified Jordan -\nBran
s - Dicke theory\, inflationary solutions are constructed by taking into\n
account a specific scalar field for particular de Sitter models in which t
he\nUniverse is filled by the vacuum. We consider the inflationary expansi
on\nfrom the Planck time till the beginning of the hot stage in the case o
f a\nminimally coupled scalar field. In the first model we take a massless
scalar\nfield and in the second one - a conformally coupled scalar field.
In both\ncases there is a specific cosmological scalar that is an analogo
us of the\nvariable cosmological constant.\n\nhttps://indico.cern.ch/event
/360350/contributions/854751/
LOCATION: Small Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854751/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Crystalline chiral condensates as a component of compact stars
DTSTART;VALUE=DATE-TIME:20150930T180000Z
DTEND;VALUE=DATE-TIME:20150930T184000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854729@indico.cern.ch
DESCRIPTION:Speakers: Stefano Carignano ()\nCould crystalline chiral conde
nsates form in the core of compact stars? Can their existence be determine
d through astrophysical observations? In my talk\, I will try to partially
answer these questions. For this\, I will first discuss the influence of
some realistic astrophysical conditions on the mechanism of inhomogeneous
chiral symmetry breaking and the structure of the energetically favored st
ate of quark matter. I will then discuss possible observables related to t
he formation of crystalline condensates\, with a particular emphasis on th
e effects on the equation of state of dense quark matter and its consequen
ces on the resulting mass-radius sequences for compact stars.\n\nhttps://i
ndico.cern.ch/event/360350/contributions/854729/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854729/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Extended time-dependent Ginzburg-Landau equations for rotating two
-flavor color superconductors
DTSTART;VALUE=DATE-TIME:20151002T184000Z
DTEND;VALUE=DATE-TIME:20151002T192000Z
DTSTAMP;VALUE=DATE-TIME:20190922T165057Z
UID:indico-contribution-360350-854754@indico.cern.ch
DESCRIPTION:Speakers: Karen Shahabasyan (Yerevan State University)\nWe dis
cuss an extension of the time-dependent Ginzburg-Landau equations for rot
ating two-flavor color superconducting quark matter derived earlier. The e
xtension treats the coefficient of the time-dependent term in the Ginzbur
g-Landau equation as complex number\, whose imaginary part describes non-d
issipative effects. We derive time- dependent London type equation for the
color-electric potential which obtains an additional time-dependent contr
ibution from this imaginary part. This additional term describes non-dissi
pative propagation effects. In addition we derive general expressions for
the energy flux and the dissipative function of the system.\n\nhttps://in
dico.cern.ch/event/360350/contributions/854754/
LOCATION: Main Hall\, Guesthouse
URL:https://indico.cern.ch/event/360350/contributions/854754/
END:VEVENT
END:VCALENDAR