text:
\section{Introduction}
Current radial velocity surveys have led to the discovery of over 150
extrasolar planets around main-sequence stars \citep[see][]{marcy05,mayor04}.
 The large majority of these planets  are probably gas giant
planets, as their masses are above $100 M_\oplus$. Such a collection
provides a good data set for comparing predictions of theories of planet
formation \citep[e.g.][]{ida04a,ida04b,alibert05,kac05}.

The standard model for the formation of giant planets is the
core-accretion, gas capture-model. The numerical calculations of
\citet{pollack96} show, that the formation of a giant planet in this
model can be divided into three phases. During the first one, the
solid core is formed by the collisional accumulation of
planetesimals. The second phase begins when the core reaches the mass
of a few Earth masses and starts to accrete a significant amount of
gas. During this phase the envelope stays in quasi - static and
thermal equilibrium, as the energy radiated by the envelope is
compensated for by the energy released by accreted planetesimals. As
during this phase the protoplanet accretes gas with a higher rate than
solids, the mass of the envelope finally becomes equal to the mass of
the core. At this moment phase 3 begins, during which the planet
rapidly grows in mass by runaway accretion of gas. The final mass and
location of a giant planet are determined by its gravitational
interaction with its environment. As it grows in mass it induces
spiral waves in the gaseous disk. This leads to the transfer of
angular momentum resulting in the inward migration of the planet and
possibly in the gap opening \citep{lin86,lin96,ward97}. This last
phenomenon strongly reduces the further growth of the planet.

The main problem with that scenario is related to the timescale
required to form a giant planet in it. In general it is the same order
of magnitude as the lifetime of the protoplanetary disk, and it is not
necessarily certain if the giant planet is able to form before
dispersion of the disk.  Close to the star, the formation time of a
giant planet in the gas capture model is determined by phase 2, while
at larger distances ($\gtrsim 10 \mr{AU}$) the lengths of phases 1 and
2 become comparable. The lengths of these two phases depend on the
initial surface density of the planetesimal swarm in the given
location. The larger the density, the faster the core grows and
reaches higher mass at the end of phase 1. With the higher mass of the
core, the length of phase 2 also diminishes. In general, at every
distance from the star there is a critical value of the surface
density of planetesimals which enables formation of a giant planet
before dispersion of the protoplanetary disk; for a more detailed
discussion see \citet{kac_mass}.

However, the density of the protoplanetary swarm is not in a simple
relation with the density of gas in the disk from which it
emerges. While the gaseous component evolves in a viscous way, the
evolution of the solid component is governed by processes of gas drag,
coagulation, sedimentation, and evaporation \citep{weiden93}.  A
significant redistribution of solid material takes place in the
result, and in the inner parts of the disk its surface density can be
significantly enhanced compared to the initial value
\citep{sv97,weiden03}. Consequently, analysis of the possible masses
and orbits of giant planets resulting from the core accretion scenario
should also include the global evolution of solids in protoplanetary
disks. A simple model of this evolution was proposed by \citet{kac1}
and further extended by \citet{kac2} and \citet{kac05} to include
subsequent formation of giant planets.

In this paper we extend our models to also include the effects of
migration and the gap opening by the planet. It
enables us for the first time to characterize the distribution of
planetary masses and final locations resulting from the core accretion model,
not only including  the growth of the planet but also the preceding
evolution of solids, which determines the surface density of the
planetesimal swarm. In Sect. \ref{s:methods} we explain our approach
to the evolution of the protoplanetary disk and planet formation. The
results are presented in Sect. \ref{s:results} and discussed in Sect. \ref{s:concl}.

\section{Methods}
\label{s:methods}
In our approach we divide the formation of giant planets into three
phases in a natural way. In the first one the planetesimal swarm is
formed in the protoplanetary disk by the collisional accumulations of
solids. This phase lasts till the gravitational interactions between
solid bodies become the dominant factor governing their evolution. In
the second epoch the giant planet is build by the accretion of the
planetesimals, and at later stages of gas onto the protoplanetary
core. Finally, when the mass of the planet reaches a critical value,
the planet migrates within the disk and reaches its final position. We now
discuss how we modeled each of these phases.

\subsection{Formation of a planetesimal swarm}

We describe the protoplanetary disk as a two-component fluid
consisting of gas and solids. We modeled the gaseous component as a
geometrically thin turbulent $\alpha$ disk \citep{73aa24_337}. Its
surface density $\Sigma$ is given as a function of distance $a$ from
the star and time $t$ in terms of a selfsimilar solution of
\citet{s98}. All other quantities characterizing the gas were obtained
by solving the standard set of equations for a thin-disk approximation
\citep[e.g.][]{accr_power}. The initial conditions were parameterized
by two quantities: the initial mass of the disk $M_0$ and its initial
outer radius $R_0$.

The crucial approximation underlying our approach to the evolution of
solids is that the size distribution of particles at any given radial
location is narrowly peaked around a mean value particular to this
location and time. In the practical implementations it means that
sizes of the particles $s$ are expressed as a single-value function of
time and position, $s=s(t,r)$.
 Collectively, all solid particles are
treated as a turbulent fluid characterized by its mean surface
density $\Sigma_{\rm s}(t,r)$, which is governed by the continuity equation:
\begin{equation}
\frac{\partial \Sigma_{\rm s}}{\partial t} +
\frac{1}{r}\frac{\partial}{\partial r}(r V_{{\rm s}} \Sigma_{\rm s})=0
\mr{.}
\label{dustEvolution}
\end{equation}
The radial drift velocity of solids $V_{\rm s}$ is the result of the
frictional coupling between solids and the gas and depends on the local
size of the particles and properties of the gas. In the regions where
the temperature of the disk is higher than the evaporation temperature
$T_\mathrm{evap}$, the solids are treated as vapour with a velocity
equal to the velocity of the gas.

The size of the
particles is governed by the second equation:
\begin{equation}
\frac{\partial \Sigma_{\rm size}}{\partial t} +
\frac{1}{r}\frac{\partial}{\partial r}(r V_{{\rm s}} \Sigma_{\rm size}) = f \Sigma_{\rm s}
\label{sizeDustEvolution}
\end{equation}
where $\Sigma_\mathrm{size}=s \Sigma_{\rm s}$.  The source function $f$
describes the growth of particles due to mutual collisions and
subsequent coagulation.
The main assumptions used in its derivation are that all collisions
between particles lead to coagulation and that the relative velocities
of colliding particles are given by the turbulent model described by
\citet{sv97}.  In the calculation of the density of solids from their surface
density, the effect of their sedimentation toward the midplane of the
disk is taken into account by evolving the scale height of the solid disk.

Initially the surface density of solids is everywhere a constant
fraction of the surface density of gas, and their sizes amount to
$10^{-3}\ \mathrm{cm}$. The results discussed in the subsequent
sections do not depend on the choice of that particular value, as long
as the solids are initially small enough to couple well to the gas.

\subsection{Growth of planets}
\label{s:growth}
Our procedure for the formation of the giant planet starts when the
planetesimals at a given point in the disk reach radii of $2\
\mr{km}$. That moment determines the initial surface density of the
planetesimal swarm.  The growth of the protoplanetary core is described by
the following formula given by \citet{papaloizou99}:
\begin{equation}
\dot{M_\mathrm{c}}=C_1 C_\mathrm{cap} R_\mathrm{p} R_\mathrm{H} \Omega_\mathrm{K}
\Sigma_\mathrm{s}
\label{eq:mc}
\end{equation}
where
\begin{equation}
R_\mathrm{H}=a\left(\frac{M_\mathrm{p}}{3 M_\star}\right)^{1/3}
\end{equation}
is the radius of the Hill sphere of the planet and $\Omega_\mr{K}$ the
Keplerian angular velocity.  The value of $C_1$ given by
\citet{papaloizou99} is $81\pi/32$; we use a factor of 5 (the
difference comes from the different definition of $R_\mathrm{H}$).
The quantity $C_\mathrm{cap}$ describes the increase in the effective
capture radius of the planet within respect to its real radius
$R_\mathrm{p}$ due to the interaction of planetesimals with the
envelope of the planet \citep{podolak88}. We use for it an approximate
fit provided by \citet{hubickyj01}, made to the results of
\citet{boden00}. For those core masses that are less then $5
M_{\oplus}$, no increase in the effective capture radius is assumed,
i.e. $C_\mathrm{cap}(M_\mathrm{c}<5M_\oplus)=1$. For larger core
masses, it increases linearly with the mass of the core, reaching its
maximum value of $C_\mathrm{cap}=5$ for $M_\mathrm{c}=15 M_\oplus$. We
assume that the surface density of planetesimals $\Sigma_\mr{d}$ is
constant throughout the feeding zone which, extends to 4 Hill radii on
both sides of the planetary orbit. Furthermore, $\Sigma_\mr{d}$
changes only due to accretion of the planetesimals onto the core and
the growth of the feeding zone.

Significant accretion of gas onto the core begins when it reaches
a critical mass of
\begin{equation}
M_\mathrm{c,crit}= 10 \left(\frac{\dot{M}_\mathrm{c}}{10^{-6}
  \ M_\oplus\ yr^{-1}}\right)^{0.25}
\left(\frac{\kappa_\mathrm{env}}{1\ \mathrm{cm}^2\ \mathrm{g}^{-1}}\right)^{0.25}
\label{e:mcrit}
\end{equation}
\citep{ikoma00}, where $\kappa_\mathrm{env}$ is the opacity in the
envelope of the planet. Its actual magnitude is currently poorly
constrained. We assume that $\kappa_\mathrm{env}=1\ \mathrm{cm}^2\
\mathrm{g}^{-1}$. When the mass of the protoplanet exceeds
$M_\mathrm{c,crit}$, it contracts on the Kelvin-Helmholtz time scale
$\tau_\mathrm{KH}$.  By fitting the result of
\citet{pollack96} \citet{bryden00} show that
\begin{equation}
\tau_\mathrm{KH}=10^{b} \left(\frac{M_\mathrm{p}}{M_\oplus}\right)^{-c}
    \left(\frac{\kappa}{1 \mathrm{cm^2\ g^{-1}}}\right)\ \mathrm{yr}
\end{equation}
where the exponents  $b=10$ and $c=3$. However, the gas accretion
rate connected with this contraction cannot be higher than the speed
with which viscous transport of gas replenishes the feeding zone of the
planet.  Consequently, we adopt the
following equations for the gas accretion rate onto the star
\begin{equation}
\frac{\mathrm{d} M_\mathrm{env}}{\mathrm{d}t} =
  \min \left[\frac{M_\mathrm{p}}{\tau_\mathrm{KH}}, \dot{M}_\mr{disk} \right]
\label{eq:menv}
\end{equation}
where $\dot{M}_\mr{disk}$ is the accretion rate in
the disk without the planet. We assume that it is equal to $\pi
\alpha C_s H \Sigma$, where $C_S$ is the sound speed in the gaseous
disk, $H$ its scale height, and $\Sigma$ its gas surface density at the given
location.

When the Hill radius of the planet becomes larger than 1.5 of the scale
height of the disk, the planet induces a strong tidal torque on the
disk and opens a gap in it. As a  result the accretion of gas is
strongly diminished. Its maximum rate is then equal to:
\begin{equation}
\dot{M}_\mr{env}= \dot{M}_\mr{disk} \left\{1.668
\left(\frac{M_\mr{p}}{M_\mr{J}}\right)^{1/3} \exp \left[-\frac{M_\mr{p}}{1.5
M_\mr{J}}\right]+0.04\right\}
\end{equation}
where $M_\mr{J}$ is the Jupiter mass \citep{veras04}.

\subsection{Migration}
\label{s:migr}
The gravitational interaction of a planet with the disk leads to its
migration and to formation of the gap in the disk \citep{lin86,ward97}.
For a low-mass planet the interaction is linear and results in
so-called type~I migration. In contrast to this scenario, high-mass planets
open a gap in the disk that reduces the timescale of migration
(referred to as type II migration).

Analytical calculations show that the timescale of type I migration in
a laminar disk is much shorter than both the disk lifetime and the
timescale of planet formation. Consequently, if type I migration has taken
place, nearly all planets would be accreted onto the star and the
probability of finding any planetary system would be very
low. Likewise, recent simulations by \citet{nelson04} suggest that
the torques exerted onto a low mass planet in a turbulent MHD disk
fluctuate strongly. As a result the planet proceeds at a random walk
and the mean value of the migration velocity is highly reduced. Due to
these uncertainties we neglect the type I migration in our models.

Type II migration begins when the planet is massive enough to open
a gap in the gas. It happens when the Hill radius of the planet is
larger than 1.5 of the disk scale height. If the mass of the planet is
negligible in comparison to the mass of the disk, the inward velocity of
the planet is regulated by the viscosity of the disk \citep{ward97}:
\begin{equation}
\frac{\mathrm{d} a}{\mathrm{d} t} = - \alpha \frac{C_\mathrm{s}^2}{a \Omega_\mathrm{k}}
\label{e:tIIs}
\end{equation}
where $C_\mr{s}$ is the sound velocity in the gas. In the case of a
planet with a larger mass than the mass of the disk, the migration
is slowed down. The variation in the planetary angular momentum is
then equal to the angular momentum transport rate in the disk \citep{lin96}:
\begin{equation}
\frac{\mathrm{d}}{\mathrm{d} t} [M_\mathrm{p} a^2 \Omega_\mathrm{k}]
= - \frac{3}{2} \nu \Sigma  \Omega_{\rm k} a^2 \ .
\label{e:tIIl}
\end{equation}
 In our calculations we used the smaller of the values of
$\mathrm{d}a/\mathrm{d}t$ given by Eqs. (\ref{e:tIIs}) and
(\ref{e:tIIl}). The migration of the planet was calculated using the
4th order Runge -- Kutta method. It stops when either the time
from the beginning of the calculation (including the time needed for
the formation of the planetesimal swarm) is longer then the lifetime of
the protoplanetary disk $\tau_\mathrm{f}$, or the orbit of the planet becomes
smaller than $0.01~\mr{AU}$. In the latter case we assumed that the planet
is accreted onto the star. In our calculations $\tau_\mathrm{f}=3\times 10^6\
\mr{yrs}$, which  agrees with  observations \citep{haisch}.

\section{Results}
\label{s:results}
Using the methods described in the previous section we were able to
investigate the range of masses and orbits of giant planets which are
able to form in protoplanetary disks characterized by different
initial conditions.  First, we calculated a grid of models of
protoplanetary disks. Every model is characterized by two parameters:
the initial mass ($M_0$) and outer radius ($R_0$) of the gaseous disk.
 Their initial masses are uniformly distributed
between 0.02 and 0.2 $\mathrm{M_\odot}$. The range of outer radii was
chosen with the goal of including all models in which the formation of giant
planets is possible. The number of radii is constant per interval of
$\lg R_0$.  The viscosity parameter $\alpha$ is equal to 0.001 for all
models. The solids consist of water ice with a bulk density of $1\,
\mathrm{g\,cm^{-3}}$ and have an evaporation temperature of $150\,\mr{K}$.
For every value of $[M_0, R_0]$ we also checked the gravitational stability
of the corresponding gaseous disk. In some cases the value of the Toomre
parameter
\begin{equation}
  Q=\frac{C_\mathrm{S} \Omega_\mathrm{K}}{\pi G \Sigma}
\end{equation}
drops below 1 in the outer regions of the disk. It means that they are
gravitationally unstable with respect to the axisymmetric modes. We
assumed that these parts of the disk fragment and some giant planets
are formed there on a very short time scale \citep[see
i.e.][]{boss02}. Consequently we used modified initial values of the
mass and outer radius of the disk, which correspond to the mass and
size of the stable part of the original disk. Our distribution the of
initial parameters of protoplanetary disks is an \emph{artificial}
one. In general one should use the distribution that occurs in
nature. Unfortunately current observations do not provide such
information. However, our results remain valid, as we are interested
only in characterizing the general set of possible orbital sizes and
masses of planets.

Using that grid of evolved models we performed Monte-Carlo
calculations to produce the $M_p - a$ distribution of planets
resulting from our models. With the uniform probability we randomly
chose one of the models from the calculated grid. Next, we chose the
initial distance of the planet from the star $a$ with constant
probability per interval of $\lg a$.  We evolved the mass and semimajor
axis of the planet according to the equations given in
Sects. \ref{s:growth} and \ref{s:migr}, starting from the time at which
the planetesimals at radial distance $a$ reach a radius of $2
\mathrm{km}$ in the given model of the protoplanetary disk.  To better
illustrate how the type II migration and the accretion of gas after
opening the gap change the parameters of the giant planets we also
performed calculations in which those two phenomena were not
included.

The results of calculations in which the planets were neither
permitted to increase their masses after the gap opening  in the
disk or to change their semimajor axes are presented in the upper panel
of Fig. \ref{f:ice}.
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics[]{ice_new.ps}}
\caption{The distribution of theoretically predicted semimajor axes
  and masses of planets around a star with a mass of $1 M_\odot$.  The
  upper panel shows planets that neither migrate nor grow in mass
  after they are massive enough to open the gap in the disk. The lower
  one presents results for planets that undergo type II migration,
  but do not grow after gap opening. The solid material in the disk
  is water ice.}
\label{f:ice}
\end{figure}
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics[]{schem.ps}}
\caption{The schematic diagram of  distribution of theoretically predicted semimajor axes
  and masses of planets around a star with a mass of $1 M_\odot$
  without effects of the gap opening and subsequent accretion of gas
  onto the planet.}
\label{f:schem}
\end{figure}
It shows that the planets can be divided into two main groups (see
also Fig. \ref{f:schem}). In the first one there are bodies with
masses smaller than $\sim20 M_\oplus$. These bodies were not able to
accrete a significant amount of gas so the nearly only consist of
their solid cores.  In the second group, there are planets with masses
larger than $\sim100M_\oplus$.  In these cases the runaway gas accretion
 has already taken  place and the majority of their masses are in the form of
gaseous envelopes. They are massive enough to open a gap in the disk.
The small number of planets with intermediate masses results from the
fact that, as the mass of the planet grows above $\sim 20 M_\oplus$, the
timescale of the accretion of gas quickly becomes much shorter than
the lifetime of the protoplanetary disk.  Consequently, the probability of
the disk to disperse before the planet grows sufficiently to open a
gap  is very low \citep[see][]{ida04a}.

The giant planets in this set of models form in a region between 1 and
20~AU from the central star. They can be divided into two subgroups,
each of them forming one of the wings of the V-like shape of the
distribution of giant planets on the $a - M_p$ diagram. As the final
mass of the giant planets in this set of models is determined by
equation
\begin{equation}
M_\mathrm{p}=3 \left(\frac{1.5 H}{a}\right)^{1/3} M_\star \ ,
\end{equation}
 those two subgroups of planets reflect different ways in which the
$H/a$ ratio depends on distance from the star $a$ at the moment of gap
opening. Giant planets at distances larger than $\sim 10 \mr{AU}$ are
at that time in the optically thin parts of the planetary disk in
which $(H/a) \sim a^{7/20}$ \citep[see][]{s98}. Consequently, the
masses of these planets are correlated with their distances from the
star. The correlation is extremely narrow because scale height of the
disk does not depend on its initial mass and outer radius in this
regime in the used model of the gaseous disk.  Giant planets at orbits
smaller than $\sim 10$ AU in the moment of gap opening are in the
optically thick part of the disk in which $(H/a) \sim a^{-1/4}$, so in
their case their masses are anticorrelated with the distance from the
star. The spread of this correlation is larger, because in that case
the exact form of the $H(a)$ relation depends on the initial mass and
radius of the underlying disk. This subgroup contains the most massive,
closest planets formed in this set of simulations. They have masses
around $450 \mathrm{M_\oplus}$ and orbits around 4 AU.

In the next set of models we include the effects of type II migration,
while planets still do not accrete any more after gap opening. The
dependence of the masses of the planets resulting from this
simulations on the sizes of their orbits is presented in the lower
panel of Fig. \ref{f:ice}.  As expected, the only differences in
comparison with the previous case are in the region of the giant
planets. Moreover, the range of the masses of these planets in both
figures are the same. Giant planets at larger orbits open the gap
later because the process of their formation is longer due to lower
densities of planetesimal swarm and smaller Keplerian frequencies (see
Eq. \ref{eq:mc}). Consequently the changes in their orbits are smaller
as they have less time to migrate. Also the accretion rate in the disk
that determines the speed of migration is lower at later times. In
our calculations, only planets at orbits smaller than $\sim 9$ AU are
able to shrink their orbits by a factor larger than 10\%. As the result,
the distribution of planets on the $a - M_p$ diagram for $a> 9$ AU is
nearly the same as in the case without migration. In the case of
planets formed at smaller distances from the star, some of them are
able to migrate to orbits as small as $\sim 2$AU. Additionally, more
massive planets tend to shrink their orbits by a larger factor. This
can be explained by the higher rate of migration in the hotter
disks. At the same time such disks have larger scale heights, and
giant planets can reach larger masses before gap opening and
stopping  their growth. All these factors lead to the small spread
of giant planets around a curve on the $a-M_p$ diagram.
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{ice2_new.ps}}
\caption{Effect of planet growth after gap opening on the
  theoretically predicted distribution of orbital sizes and masses of
  planets around a star with mass of $1 M_\odot$. The upper panel
  shows the results for planets that undergo type II migration and
  growth after gap opening.  The lower one shows results for planets
  that undergo type II migration, but not grow after gap opening. The
  solid material is water ice.}
\label{f:ice2}
\end{figure}

In the third set of calculations, the planets both migrate and grow in
mass after gap opening.  The distribution of the resulting planets is
shown in Fig. \ref{f:ice2}. The range of their final semimajor axes is
similar to the one in the previous set of models. The maximum size of
planets at the given distance is $\sim 2000 M_\oplus$ at 2 AU and
decreases to $\sim 400 M_\oplus$ at 17 AU. The increase in the masses
of the planets, after gap opening tends to be anticorrelated with
the semimajor axes of their orbits. We explain this fact as follows.
The rate at which a giant planet accretes gas at this stage of its
evolution is determined by the accretion rate in the disk, and as such
does not strongly depend on the distance from the star. At the same
time the protoplanetary cores at smaller distances grow on shorter
timescales. There are two reasons for this. First, the accretion rate
 of planetesimals onto the core is proportional to Keplerian
frequency; second, the surface density of the nascent planetesimal
swarm tends to be larger closer to the star. Consequently,
protoplanets at smaller orbits are able to start accreting
significant amounts of gas for a longer time before dispersion of the
disk. Additionally, the accretion rate in the disk, which determines
the accretion rate of gas onto the planet, is larger in this earlier
epoch. As a result, the maximum size of the planet is everywhere a
decreasing function of the distance from the star, even in those regions
where the relation was the opposite at the moment of gap opening.

Next, we investigate how the relation between the mass of the planet
and semimajor axes of its orbit depends on the sort of material solids
consist of. For this purpose we performed similar simulations to those
described above, but with solids made of high temperature silicates
instead of water ice. For the evaporation temperature of silicates we
adopted a value of 1350~K, and for their bulk density
$3.3\,\mathrm{g\,cm^{-3}}$. The upper panel of Fig.~\ref{f:ht}
presents the distribution of planets resulting from these
calculations.
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{ht_new.ps}}
\caption{Effect of different kinds of material that the solids in
  the protoplanetary disk consist of on the theoretically predicted
  distribution of orbital sizes and masses of planets around a star
  with a mass of $1 M_\odot$. The upper panel shows the results from models in
  which solids are composed of silicates, the lower one -- from water
  ice.  In both cases the planets undergo type II migration and grow
  after gap opening.  }
\label{f:ht}
\end{figure}
Because the solids can survive at higher temperatures than ice, the
giant planets in that case can form closer to the star. Because the
rate of migration does not depend on the composition of solids,
their final orbits can also be smaller. At the same time, the distribution
of the final surface densities of the planetesimal swarms, as a
function of the distance from the star, seems to be a natural extension
of this distribution in the case of water ice solids. As a result, the
relation of $a - M_p$ for planets with silicate cores at orbits
smaller then 6 AU is just an extension to smaller values of $a$ of the
same relation for planet with water ice cores.

Consequently, in our models the most massive planets (with $M_p\sim
5000 M_\oplus$) tend to be located closest to the star at orbits with
semimajor axes $\sim ~ 0.5\,\mr{AU}$. On the other hand, planets with
silicate cores at orbits larger than $6\,\mr{AU}$ tend to have smaller
masses than their ice core counterparts. The reason is that at these
distances the time during which the core of the protoplanet only
accretes solid material becomes a significant fraction of the whole
time of its formation. The rate of the accretion of planetesimals onto
the core with the same mass, but composed of more dense material, is
lower due to its smaller physical dimensions. As a result, planets
with silicate cores start their gas accretion later and grow to
smaller masses before the dispersion of the disk. At distances larger
than $\sim 8$ AU, we do not obtain any giant planets with silicate
cores.

Finally, we investigated the influence of the central star mass on the
relation between masses and  orbit sizes  of giant planets. In
Fig. \ref{f:0.5} we present the results for two values of the stellar
mass: 0.5 and 1 $M_\odot$.
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{0.5_new.ps}}
\caption{The distribution of theoretically predicted semimajor axes
  and masses of planets around stars with masses of $1 M_\odot$ (lower
  panel) and $0.5 M_\odot$ (upper panel).  In both cases the planets
  undergo type II migration and grow after gap opening.}
\label{f:0.5}
\end{figure}
The planets around less massive stars also tend to be less massive and
have slightly smaller orbits. The first fact is explained by the lower
accretion rates in these disks, as these rates also determine the
maximum rate at which the planet can accumulate gas. The tendency of
giant planets to form around less massive stars at smaller radii is
the result of (a) a more effective radial redistribution of solids in
the disk prior to the formation of planetesimals and, as a result the
higher surface density of the planetesimal swarm, (b) a lower value of
the minimal surface density for the formation of a giant planet around
less massive stars at orbits smaller than $\sim 10$ AU
\citep[see][]{kac_mass}.

\section{Conclusions}
\label{s:concl}
We have presented the results of simulations describing the formation
of giant planets. Our model include all important phases of the
core-accretion scenario, beginning from the formation of the
planetesimal swarm from smaller solids, until the gap opening in the
disk and subsequent planet migration. We presented the distribution of
$a-M_\mr{p}$ for planets resulting from our models for a set of
different initial masses and sizes of the protoplanetary disk and for
the place of planet formation. However, our results cannot be compared
in a simple way to data for extrasolar planets, because of the lack of
knowledge of the distribution of the initial parameters of
protoplanetary disks that occur in nature. Instead our aim was to
characterize the relationship between the final orbital radii and
masses of planets that are in general possible to obtain and to check
how the resulting $a-M_\mr{p}$ distribution changes when including
different physical processes such as migration and gas accretion by
the planet after gap opening. We also investigated whether the
distribution of giant planets is mainly determined by the parameters
of the gaseous disk or the distribution of the planetesimal swarm.

We have shown that, if we do not include the effects of migration nor
accretion of gas by the planet after gap opening, the $a-M_\mr{p}$
distribution for giant planets is mainly determined by the parameters
of the gaseous disk. In that case one is able to read the information
about the dependence of the scale height of the gaseous disk on the
distance from the star from the distribution of giant planets. The
minimal and maximal distance from the star gives information about the
surface density of planetesimal swarm at those places.

By including migration in our models, reconstructing the
the properties of the gaseous disk from the distribution of giant
planets becomes more difficult. The distance that the  planet can move inward
depends not only on the gaseous environment but also on the
time between gap opening  and dispersion of the disk. But the
first of these two moments is determined by the surface density of
planetesimal swarm. This, on the other hand, is not related in a simple way
 to the local parameters of the gaseous disk. Our simulations
show that the simple reconstruction of the scale height of the gaseous
disk is possible only from distribution of giant planets at greater distances
 than $\sim 8\,\mr{AU}$, as planets at such large orbits did not
significantly move away from their original places.

If we include in our models  that the planet can still grow in
mass after gap opening, it is even more difficult, if at all possible,
to derive conclusions about the gaseous disk (its temperature, scale
height, etc.) based on the distribution of giant planets.  This is
because the rate of this additional accretion onto the planet depends
mainly on the accretion rate in the disk, while the time frame in
which this accretion can occur is determined by the surface density of
the planetesimal swarm.  The effect of the additional growth of the planet can
even lead  to reversion of the correlation between the masses of the
planets and semimajor axes of their orbits.

We also checked how the  mass of the central star influences the
distribution of planets. The main result is that in disks around less
massive stars, giant planets at the given location tend to be less
massive. At the same time, the giant planets with a given mass tend
to form closer to the less massive stars.

Our models can be seen as an extension of previous calculations
performed by \citet{ida04a} and \citet{alibert05}. In comparison, the
surface density of the planetesimal swarms in our models are computed
self-consistently. This additional factor makes it much more difficult
to predict the  structure of the gaseous disk from the distribution
of giant planets much more difficult. Nevertheless it does seem
necessary. Whenever we performed the similar calculations as
described above, but with the assumption that the surface density of the
planetesimal swarm is always a constant fraction of the surface
density of gas, we were not able to perceive any giant planets. This
seems  contradict  the results of those two papers. A
possible reason for this different result may be the difference in the
underlying models of the gaseous disk. However, we think that the main
factors are the different times for the dispersion of the gaseous disk
(3 Myr vs. 10 Myr) and the different sizes of solids at time 0 (small
grains vs. planetesimal sizes). Our models show that the time needed
to reach planetesimal sizes can be as long 1~Myr and is not
negligible.

Our results also seem to contradic observations that show that more
massive planets tend to be located farther away from the host
star. This correlation is reproduced better by the calculations of
\citet{ida04a}, who conclude that maximal mass of the planets after
including type II migration does not strongly depend on the size of
the orbit. On the other hand, in the results from \citet{alibert05}
the correlation is identical to ours, namely the more massive planets
tend to be closer to the star. This difference can have two
sources. First, \citet{ida04a} neglect the accretion of gas onto the
planet, after it opens a gap in the disk. The second reason, which we
think is more important, can again be the difference in the structure
of the gaseous disk.  In our calculations ratio $(H/r)$ is mainly a
decreasing function of the radius in the inner parts of the disk,
while it is an increasing function in the disk model of
\citet{ida04a}. Because this ratio determines the mass of the planet
which in turn is able to
open a gap in the disk, then it can play a big role in determining the
properties of the set of giant planets.

\begin{acknowledgements}
This project was supported by the German Research Foundation (DFG)
through the Emmy Noether grant WO 857/2-1 and the European
Community's Human Potential Programme trough the contract
HPRN-CT-2002-00308, PLANETS. KK acknowledge the support
from the grant No. 1 P03D 026 26 from the Polish Ministry of
Science.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


A national 'Treatment as Prevention' programme for hepatitis C has today reported high levels of cure but found that homelessness more than doubles the chance of failing treatment with direct-acting antiviral (DAA) drugs. First results from the Treatment as Prevention for Hepatitis C (TraP HepC) initiative in Iceland, which were reported today at The International Liver Congress™ 2019 in Vienna, Austria, indicate that a cure from HCV infection can be achieved with one course of treatment in almost 90% of programme participants, although cure rates may be lower among injection drug users.
According to Dr Gottfredsson, in the ITT analysis the overall cure rate after the first treatment attempt was 89.2%. Cure was achieved in a significantly smaller proportion of the cohort reporting injection drug use within the past 6 months (82.9%) compared with the cohort without recent injection drug use (92.4%; p<0.0001). Individuals with recent injection drug use were more likely to discontinue treatment (15.2% vs. 4.5%; p<0.0001), however, even when the analysis was restricted to those who completed treatment, the chance of cure was lower among those with recent injection drug use (89.9% vs. 95.3%; p=0.025).
Homelessness was associated with a greater chance of persistent viraemia at ≥12 weeks, with a relative risk (RR) of 2.42 (95% CI 1.34, 4.37; p=0.007), while living in a halfway house was associated with a lower risk (RR 0.37; 95% CI 0.12, 1.16; p=0.068).
'This is an important study, since it demonstrated the feasibility of treating this group of patients, although with a lower rate of success' said Professor Helena Cortez-Pinto from the Hospital Universitário de Santa Maria, Lisbon, Portugal, and an EASL Governing Board member.
Alter MJ. HCV routes of transmission: what goes around comes around. Semin Liver Dis. 2011;31(4):340–6.
Martin NK, et al. The hepatitis C virus epidemics in key populations (including people who inject drugs, prisoners and MSM): the use of direct-acting antivirals as treatment for prevention. Curr Opin HIV AIDS. 2015;10(5):374–80.
Wiessing L, et al. Hepatitis C virus infection epidemiology among people who inject drugs in Europe: a systematic review of data for scaling up treatment and prevention. PLoS One. 2014;9(7):e103345.
Olafsson S, et al. Treatment as Prevention for Hepatitis C (TraP Hep C) – a nationwide elimination programme in Iceland using direct-acting antiviral agents. J Intern Med. 2018;283(5):500–7.


text:
Heather Headley (Barataria, 5 oktober 1974) is een Amerikaanse zangeres, songwriter, producent en actrice, afkomstig uit Trinidad en Tobago.

Biografie
Heather Headley kon op 4-leeftijd piano spelen. De dochter van een pastoor kwam tijdens haar jeugd in aanraking met verschillende muziekstijlen en raakte geïnteresseerd in de richting van calypso, reggae en soca. Op 15-jarige leeftijd verhuisde ze met haar gezin naar de Fort Wayne, Indiana, waar haar vader nieuwe carrièremogelijkheden zag. Na haar afstuderen aan de middelbare school schreef Heather Headley zich in aan de Northwestern University op het gebied van communicatie en muziektheater. Aan het einde van haar studie besloot ze echter om geen academische carrière te maken en werd ze lid van een theatergroep. Al tijdens haar studie stond ze op het theaterpodium: ze speelde een rol in de toneelstukken Dreamgirls en The World Goes Round in het Marriott Lincolnshire Theatre.

In 1997 kreeg ze haar eerste rol in het theater. Het Disney-gezelschap gaf haar de rol van Nala in de musical The Lion King. Hierdoor kon ze de publieke aandacht op zichzelf vestigen. Kort daarna werd ze gecontracteerd door RCA Records en wijdde ze zich aan de muziekindustrie. Een jaar later zong ze samen met Kenny Lattimore het nummer Love Will Find a Way voor de musical The Lion King II, die ook in de advertentie voor deze musical werd uitgezonden. In oktober 2002 verscheen haar debuutalbum This Is Who I Am. Hoewel haar eerste single He Is werd geprezen, haalde ze de top van de hitlijsten niet. Het bereikte slechts #4 In de dancehitlijsten, maar met haar tweede single I Wish I Wasn't was ze succesvoller en haalde ze zelfs een nominatie voor de Grammy Awards. Haar album verkocht uiteindelijk een half miljoen exemplaren en kreeg goud.

In 2004 had ze een cameo in het vervolg op Dirty Dancing als zangeres. Haar tweede album My Mind kwam na een vertraging in 2006 uit. Dit album bereikte #1 in de r&b-hitlijsten. Het titelnummer werd een dancehit en als remix een #1-hit in de Amerikaanse dancehitlijsten. In hetzelfde jaar trad ze op tijdens het concert Under the Desert Sky van Andrea Bocelli en zong met hem onder meer de wereldhit The Prayer. In 2007 trad ze opnieuw op met Bocelli, dit keer in Italië in het Teatro del Silenzio bij Lajatico en zong ze opnieuw The Prayer en Vivo per lei, dit keer met een Anglo-Italiaanse versie. In 2009 verscheen haar huidige album Audience of One, waarin Headley een nieuwe muziekstijl begon: gospel.

Privéleven
Heather Headley is getrouwd met Brian Musso, een voormalig voetballer die sinds 6 september 2003 actief was bij de New York Jets.

Discografie

Singles
 2002: He Is
 2003: I Wish I Wasn't
 2006: In My Mind

Albums
 2002: This Is Who I Am
 2006: In My Mind
 2009: Audience of One
 2012: Only One in the World

Amerikaans zanger
Amerikaans liedschrijver
Amerikaans producent
Amerikaans acteur

redpajama_set_name: RedPajamaWikipedia


text:
People Technology
I do love a good password. We have to change them regularly at work and picking a new one is a fun challenge. Something secure of course. Memorable. But most importantly this is something I'll type many times every day, and each time is a chance to evoke something in myself.
It's a chance to make myself laugh, to remind myself of something, or to encourage myself. If I'm not careful it could be something that riles me up. Or I could make it into a memory exercise, or a puzzle, or a game. Your passwords will affect you; like a mantra or personal ritual, something you repeat that often is going to make its mark.
Ian Urbina of the NYT has been asking friends and strangers about their passwords.
There was the former prisoner whose password includes what used to be his inmate identification number ("a reminder not to go back"); the fallen-away Catholic whose passwords incorporate the Virgin Mary ("it's secretly calming"); the childless 45-year-old whose password is the name of the baby boy she lost in utero ("my way of trying to keep him alive, I guess").
He calls them 'keepsake passwords': mementos and reminders. There are also those that used to change:
Mauricio Estrella, a designer who emailed me from Shanghai, described how his passwords function like homemade versions of popular apps like Narrato or 1 Second Everyday, which automatically provide its user with a daily reminder to pause and reflect momentarily on personal ambitions or values. To help quell his anger at his ex-wife soon after their divorce, Estrella had reset his password to "Forgive@h3r." "It worked," he said. Because his office computer demanded that he change his password every 30 days, he moved on to other goals: "Quit@smoking4ever" (successful); "Save4trip@thailand" (successful); "Eat2@day" ("it never worked, I'm still fat," Estrella wrote); "Facetime2mom@sunday" ("it worked," he said, "I've started talking with my mom every week now").
At the other end of the password spectrum I remember a girl I went to school with whose password was 'tree'. She said it was because it was short, easy to remember, and (most importantly) all the letters were next to each other on the keyboard.
Tags nyt, passwords
← Owls → My sort of pad

redpajama_set_name: RedPajamaCommonCrawl


text:
CBFC certified films in Silent
Die Nashorner (Rhinoceroses) (Instrumental Music Only) (Celluloid) Silent U (Unrestricted Public Exhibition)
Die Schuffebrutsche (Celluloid) Silent U (Unrestricted Public Exhibition)
Die Utopen (Utopia) (Celluloid) Silent U (Unrestricted Public Exhibition)
Die Welt And Ihre Menschen (Celluloid) Silent U (Unrestricted Public Exhibition)
Die Zauberschere (The Magic Scissors) (Silhouette - Cartoon) (Celluloid) Silent U (Unrestricted Public Exhibition)
Diffusion (Celluloid) Silent U (Unrestricted Public Exhibition)
Dimensions (Celluloid) Silent U (Unrestricted Public Exhibition)
Dink Tile Sq Gold Gauage,Pack Gaskets (Celluloid) Silent U (Unrestricted Public Exhibition)
Direction Line Railroad (Celluloid) Silent U (Unrestricted Public Exhibition)
Diseases Of The Ear, Nose And Throat (Celluloid) Silent U (Unrestricted Public Exhibition)
Diseases Of The Esophagus (Celluloid) Silent U (Unrestricted Public Exhibition)
Dislocations & Stacking Faults In Stainless Steel (Celluloid) Silent U (Unrestricted Public Exhibition)
Disorder Of The Vestibular System (Celluloid) Silent U (Unrestricted Public Exhibition)
Disorders Of Coordination (Celluloid) Silent U (Unrestricted Public Exhibition)
Disorders Of Gait (Celluloid) Silent U (Unrestricted Public Exhibition)
Divine Will International Assembly Of Jehovahs Witnesses (Celluloid) Silent U (Unrestricted Public Exhibition)
Diving (Part Ii) (Celluloid) Silent U (Unrestricted Public Exhibition)
Diving Part I (Celluloid) Silent U (Unrestricted Public Exhibition)
Diving Part Ii (Celluloid) Silent U (Unrestricted Public Exhibition)
Division Of Natural Numbers (Celluloid) Silent U (Unrestricted Public Exhibition)
Division Of The Dna Molecule (Celluloid) Silent U (Unrestricted Public Exhibition)
Documentary Film On Tourism In Tamilnadu (Celluloid) Silent U (Unrestricted Public Exhibition)
Doe's Last Stand (Longer Version) (English Captions) (Celluloid) Silent U (Unrestricted Public Exhibition)
Doe's Last Stand (Shorter Version) (English Captions) (Celluloid) Silent U (Unrestricted Public Exhibition)
Dominance Neurosis And Aqqression In Cats (Celluloid) Silent U (Unrestricted Public Exhibition)
Donald And Pluto (Celluloid) Silent U (Unrestricted Public Exhibition)
Donald Duck (Eng. Subtitle) (Celluloid) Silent U (Unrestricted Public Exhibition)
Donald Duck In The High Andes (Celluloid) Silent U (Unrestricted Public Exhibition)
Doom Of Dracula (Longer Version) (Celluloid) Silent A (Restricted to adults)
Doom Of Dracula (Shorter Version) (English Captions) (Celluloid) Silent U (Unrestricted Public Exhibition)
Doors-a & P - R & E (Celluloid) Silent U (Unrestricted Public Exhibition)
Dots (Celluloid) Silent U (Unrestricted Public Exhibition)
Double Cross At Criss Cross (Celluloid) Silent U (Unrestricted Public Exhibition)
Double Cross At Criss Cross (Shortened Version) (Celluloid) Silent U (Unrestricted Public Exhibition)
Double Portrait (Music Only) (Cartoon) (Celluloid) Silent U (Unrestricted Public Exhibition)
Double Trouble (Longer Version) (Celluloid) Silent U (Unrestricted Public Exhibition)
Douglas Fairbanks The Three Musketeers (1921) (Celluloid) Silent U (Unrestricted Public Exhibition)
Down Hill (Video) Silent U (Unrestricted Public Exhibition)
Down Through The Years (Arandom Survey Of Montreal) (Celluloid) Silent U (Unrestricted Public Exhibition)
Down To The Sea (Celluloid) Silent U (Unrestricted Public Exhibition)
Down To The Sea (Following The River No 6) (Celluloid) Silent U (Unrestricted Public Exhibition)
Dr. Cyclops (Celluloid) Silent U (Unrestricted Public Exhibition)
Dr. Cyclops (Longer Version) (Celluloid) Silent U (Unrestricted Public Exhibition)
Dracula (Celluloid) Silent U (Unrestricted Public Exhibition)
Dracula (Longer Version) (English Captions) (Celluloid) Silent U (Unrestricted Public Exhibition)
Dreams On Wings Part 2 (Music Only) (Celluloid) Silent U (Unrestricted Public Exhibition)
Dreams On Wings Part I (Music Only) (Celluloid) Silent U (Unrestricted Public Exhibition)
Dreispring (Hop Step And Yump) (German Titles) (Celluloid) Silent U (Unrestricted Public Exhibition)
Druckguss I, Ii, Iii (Compressed Gas A, B, C) (Celluloid) Silent U (Unrestricted Public Exhibition)
Druckluft Flotation (Celluloid) Silent U (Unrestricted Public Exhibition)
Drug Abuse (Celluloid) Silent U (Unrestricted Public Exhibition)
Drums - India (Music Only) (Celluloid) Silent U (Unrestricted Public Exhibition)
Drunk Young Man In Distress (Video) Silent U (Unrestricted Public Exhibition)
Dubbawala (Music Only) (Celluloid) Silent U (Unrestricted Public Exhibition)
Duel (Celluloid) Silent U (Unrestricted Public Exhibition)
Duel Of The Wizards (Celluloid) Silent U (Unrestricted Public Exhibition)
Duel Of The Wizards (Eng. Sub-title) (Celluloid) Silent U (Unrestricted Public Exhibition)
Dumbo Makes The Big Top (Celluloid) Silent U (Unrestricted Public Exhibition)
Dumbo The Flying Elephant (Celluloid) Silent U (Unrestricted Public Exhibition)
Durgaraj Raigad (Titles In Marathi) (Celluloid) Silent U (Unrestricted Public Exhibition)
Dutch East Indies (Celluloid) Silent U (Unrestricted Public Exhibition)
Dyc Cassette & Cd (Video) Silent U (Unrestricted Public Exhibition)
Dynamic Response (Celluloid) Silent U (Unrestricted Public Exhibition)
Dynamics Of Respiration (Celluloid) Silent U (Unrestricted Public Exhibition)
Dynamo And Starter Operations (Celluloid) Silent U (Unrestricted Public Exhibition)
Early Activatities (Celluloid) Silent U (Unrestricted Public Exhibition)
Early Frick Films (Celluloid) Silent U (Unrestricted Public Exhibition)
Early Play (Subtitle In English) (Celluloid) Silent U (Unrestricted Public Exhibition)
Eart, Surface And Climate (Celluloid) Silent U (Unrestricted Public Exhibition)
Earth's Land And Seas (Celluloid) Silent U (Unrestricted Public Exhibition)
East African Senery Part Iii (Celluloid) Silent U (Unrestricted Public Exhibition)
East Vault And Rolling Of End Fittings West Vault (Celluloid) Silent U (Unrestricted Public Exhibition)
Easy To Carry-easy To Care (Celluloid) Silent U (Unrestricted Public Exhibition)
Easy To Cary-easy To Care (Celluloid) Silent U (Unrestricted Public Exhibition)
Eclipse Of The Sun (Celluloid) Silent U (Unrestricted Public Exhibition)
Edampsia (Celluloid) Silent U (Unrestricted Public Exhibition)
Edipse Of The Sun (Celluloid) Silent U (Unrestricted Public Exhibition)
Edison Films (1890's) (Celluloid) Silent U (Unrestricted Public Exhibition)
Education Of Movement In Third & Fourth Grade (Part 1 & 2) (English Titles Only) (Celluloid) Silent U (Unrestricted Public Exhibition)
Edwin S. Porter: Four Films (Celluloid) Silent U (Unrestricted Public Exhibition)
Eera-beeri (Celluloid) Silent U (Unrestricted Public Exhibition)
Effect Of Oxygen On Retinal Vessels (With English Sub-titles) (Celluloid) Silent U (Unrestricted Public Exhibition)
Effect Of Serpasil In A Woman Patient With Huntington's Chorea (Celluloid) Silent U (Unrestricted Public Exhibition)
Egg Production (Celluloid) Silent U (Unrestricted Public Exhibition)
Egyptian Village (Celluloid) Silent U (Unrestricted Public Exhibition)
Ehsan-trl (Celluloid) Silent U (Unrestricted Public Exhibition)
Eight Equalities (Celluloid) Silent U (Unrestricted Public Exhibition)
Einsatz Und Arbeitsweise Der Kontinuierlichen Dampfmaschine (Application And Mode Of Operation Of The Continual Patato Steming Machine) (Celluloid) Silent U (Unrestricted Public Exhibition)
Einstellen Der Zundung I Magnet Zundung (Spark Timing I )' (Celluloid) Silent U (Unrestricted Public Exhibition)
Einstellen Der Zundung Ii Batterie Zundung (Spark Timing Ii)' (Celluloid) Silent U (Unrestricted Public Exhibition)
Einstellen Der Zundung Iii (Spark Timing Iii)' (Celluloid) Silent U (Unrestricted Public Exhibition)
Eisenerzspattung Dusch Kohlen Oxyd (Celluloid) Silent U (Unrestricted Public Exhibition)
Eisenybergbau In Laffland (Celluloid) Silent U (Unrestricted Public Exhibition)
Ek - Bahen (Celluloid) Silent U (Unrestricted Public Exhibition)
Ek Rangit Kagad (Video) Silent U (Unrestricted Public Exhibition)
Ek Tha Chhotu Aur Ek Tha Motu (Titles In Hindi) (Celluloid) Silent U (Unrestricted Public Exhibition)
Ekkani (Video) Silent U (Unrestricted Public Exhibition)


text:
using System;
using Rock.StringFormatting;

namespace Rock.Logging
{
    /// <summary>
    /// Defines a <see cref="SetException"/> extension method.
    /// </summary>
    public static class SetExceptionExtensionMethod
    {
        /// <summary>
        /// Sets the value of <see cref="ILogEntry.ExceptionDetails"/> to a string representation
        /// of the provided exception. Also sets various extended properties
        /// (inner exception messages and items in <see cref="Exception.Data"/>).
        /// </summary>
        /// <param name="source">The instance of <see cref="ILogEntry"/> to set exception details for.</param>
        /// <param name="exception">The exception to be added to this instance of <see cref="ILogEntry"/>.</param>
        /// <param name="exceptionContext">Contextual information about the exception. This value
        /// should give a developer additional information to help debug or fix the issue.</param>
        /// <example>
        /// <code>
        /// ILogger logger = LoggerFactory.GetInstance();
        ///
        /// public void ProcessLoan(int loanNumber)
        /// {
        ///   try
        ///   {
        ///     LogEntry entry = new LogEntry("Doing Something");
        ///     entry.ExtendedProperties.Add("LoanNumber", loanNumber);
        ///
        ///     DoSomething(loanNumber);
        ///
        ///     if(logger.IsInfoEnabled)
        ///     {
        ///       logger.Info(entry);
        ///     }
        ///   }
        ///   catch (Exception ex)
        ///   {
        ///     if (logger.IsErrorEnabled)
        ///     {
        ///       entry.SetException(ex);
        ///       logger.Error(entry);
        ///     }
        ///   }
        /// }
        /// </code>
        /// </example>
        public static void SetException(this ILogEntry source, Exception exception, string exceptionContext = null)
        {
            if (exception != null)
            {
                source.ExceptionType = exception.GetType().ToString();
                source.ExceptionDetails = exception.FormatToString();
                source.ExceptionContext = exceptionContext;
                source.SetExtendedPropertiesFor(exception);
            }
        }

        private static void SetExtendedPropertiesFor(this ILogEntry logEntry, Exception ex)
        {
            var innerLevel = 0;

            while (ex != null)
            {
                var exceptionKey =
                    innerLevel != 0
                        ? string.Format("Inner Exception {0}: {1}", innerLevel, ex.GetType())
                        : ex.GetType().ToString();

                if (!logEntry.ExtendedProperties.ContainsKey(exceptionKey))
                {
                    logEntry.ExtendedProperties.Add(exceptionKey, ex.Message);
                }

                foreach (var dataKey in ex.Data.Keys)
                {
                    if (dataKey == null) { continue; }

                    var dataKeyString = "((" + ex.GetType() + ")Exception.Data)[\"" + dataKey + "\"]";

                    if (logEntry.ExtendedProperties.ContainsKey(dataKeyString)) { continue; }

                    var dataValue = ex.Data[dataKey];

                    var dataValueString =
                        dataValue == null
                            ? null
                            : dataValue.ToString();

                    logEntry.ExtendedProperties.Add(dataKeyString, dataValueString);
                }

                innerLevel++;
                ex = ex.InnerException;
            }
        }
    }
}

redpajama_set_name: RedPajamaGithub


text:
Q: Can I pass an array to a lambda such that I can use sizeof() I'm replacing some #defines with lambdas in my code. I have a bunch of structures which are the result of shader compilation, declared like so:
const BYTE ShaderByteCode[] =
{
     68,  88,  66,  67, 233, 176,
     42,  49,  64,  77, 131, 190,
     75,  97, 214,  59, 236, 203,
    188, 191,   1,   0,   0,   0,
    etc...
};

A #define has ShaderByteCode as an input, and calls SetPixelShader, which takes the size of the byte array as a parameter:
#define doThing(Thing, ShaderByteCode) \
Thing.SetPixelShader(ShaderByteCode, sizeof(ShaderByteCode) ); \

Using a lambda, like this:
auto doThing = [](Thing& thing, const BYTE ShaderByteCode[]) {
        thing.SetPixelShader(ShaderByteCode, sizeof(ShaderByteCode));
    };

I will just get a pointer to the start of the array and sizeof() returns the size of the pointer.
Is there a way I can pass a single parameter into the lambda, or do I need to do what I'm currently doing and pass the size in separately?

A: As suggested in comments, maybe a raw array isn't the best thing to pass here.
But you mention a #define macro which does the sizeof. If you want to keep using this because it's the official method of some API, here are some ways to get an array function parameter. The important thing is, a reference-to-array avoids the array-to-pointer decay step.
If you're using C++20, you can do
auto doThing = [] <std::size_t N> (Thing& thing, const BYTE (&ShaderByteCode)[N]) {
    THE_MACRO(thing, ShaderByteCode);
};

If you're using C++14 or later,
auto doThing = [] (Thing& thing, const auto& ShaderByteCode) {
    using deref_t = std::remove_reference_t<decltype(ShaderByteCode)>;
    static_assert(std::is_array<deref_t>::value &&
                  std::is_same<std::remove_extent_t<deref_t>, const BYTE>::value,
                  "Invalid argument type in doThing lambda");
    THE_MACRO(thing, ShaderByteCode);
};

If using C++11, or using C++14-C++17 but you need the functor to be SFINAE-friendly, I don't think it can be done with a lambda, but you could define your own functor class with templated operator().

A: Use template and let template deduction find size of the array:
template<typename T, size_t N>
void doThing(Thing& thing, const T (&shaderByteCode)[N])
{
    thing.SetPixelShader(shaderByteCode, N);
}

No macros, no boiler plate, works with quite old C++ standard. C++ will deduce the parameters for you, you do not have to type them explicitly:
Thing thing;
doThing(thing, ShaderByteCode);

some demo.

A: decltype will be your friend.
If you have whatever C-Style array, decltype will know the number of members.
For example:
using BYTE = unsigned char;
const BYTE ShaderByteCode[] =
{
     68,  88,  66,  67, 233, 176,
     42,  49,  64,  77, 131, 190,
     75,  97, 214,  59, 236, 203,
    188, 191,   1,   0,   0,   0,
    1,2,3
};
using Array = decltype(ShaderByteCode);

Array will be of type const unsigned char[27];
And with that you can pass this element per reference (or pointer) to a function or to a lambda.
This could look like for example this:
#include <iostream>

using BYTE = unsigned char;
const BYTE ShaderByteCode[] =
{
     68,  88,  66,  67, 233, 176,
     42,  49,  64,  77, 131, 190,
     75,  97, 214,  59, 236, 203,
    188, 191,   1,   0,   0,   0,
    1,2,3
};
using Array = decltype(ShaderByteCode);

void SetPixelShader(Array& sbc) {
    std::cout << sizeof(sbc) << '\t' << sizeof(Array) << '\n';
}

int main() {
    auto doThing = [](const Array& SBC) { SetPixelShader(SBC);};
    doThing(ShaderByteCode);
}

redpajama_set_name: RedPajamaStackExchange


text:
The Lies Ill-Concealed
The Lies Ill-Concealed Recap
Susan is told by her doctor that she can't have sex for six weeks following her kidney transplant. She ends up having a sexy dream about Paul and wakes up in shock. Mike reveals that she has been moaning in her sleep and, believing that she was dreaming about him, asks her for details. However, Susan manages to stop him asking by saying that she will show him when they can have sex again in two days time.
Later, Susan goes to pick up M.J. from Karen's and asks her to watch him again on Wednesday. Karen agrees, explaining that she knows that is the night Mike and Susan can have sex again. Susan is embarrassed, but as she leaves Karen points out that Susan's old house - rented by Paul - is messy. Susan goes over to check on Paul and, while she is waiting for him to answer the door, picks up his newspapers for him. She is surprised when he opens the door and she is face to face with his crotch. However, she notices that he is thin and behind on his chores and asks if he is alright. Paul insists that he is fine. Later, Susan tells Mike that Paul seems run down but Mike admits that he doesn't care, pointing out that Paul has behaved badly towards them in the past. He asks Susan to stay away from Paul. However, that night Susan has another sexy dream about Paul. At her next doctor's appointment, she asks if the dreams are normal. Her doctor suggests that her dreams are telling her to make sure Paul is all right and admits that they might not stop until she does. Susan goes to see Paul and eventually he reluctantly agrees to let her in. Susan, noticing that his house is a mess, decides to help him make a potato and leek soup. As they eat, Susan says they should start having meals together again. She suggests that Paul could become the friendly neighbor she used to have once more. Meanwhile, Mike drops off M.J. at Karen's house and is shocked to see through the window that Susan and Paul are together. He storms over there and Susan spots him. She goes outside and explains that Paul is suffering and has no-one. Mike is angry and claims that Paul is dangerous, but Susan says she doesn't need to be rescued and refuses to leave someone who is hurting. She goes back inside. Later, she returns home and is surprised to see a romantic meal laid out. Mike admits that he thought about it and realised that he can't be mad at Susan for being kind and compassionate. He carries her to the bedroom.
Lynette is thrilled when she discovers that Tom has been invited to an important leadership conference and that she can go too. When they arrive, they meet Bob and Lee. Lynette goes to stand in the line for a drink and reads the conference program over somebody's shoulder. She begins chatting to the woman holding it and explains that she is looking forward to the keynote speaker, Chris Cavanaugh. The woman agrees and introduces herself as Meg Butler, the president of Amtec. Lynette explains that she is with her husband, and Meg immediately becomes rude, explaining that Lynette won't see Chris Cavanaugh because the seminars are not available to plus ones. Lynette is surprised and Meg explains that it is because some people spent their lives working up the corporate ladder and others just married someone who did. Lynette is furious but Lee manages to drag her away. Lynette ends up attending yoga, salsa dancing and flower arranging with the other plus ones and gets more and more frustrated. Eventually, she tries to persuade the other plus ones to storm the seminars with her, saying that they are in 21st century America, not an oppressive patriarchal regime. However, the organizers quickly offer the plus ones cocktails and they are distracted. Lynette gives up and takes a drink too. Later, she finds Tom and asks if he can pull some strings to get her into the Chris Cavanaugh talk but he admits that there is nothing he can do. One of the organizers arrives and drags Lynette away to the spa. While she is there, Lynette overhears Meg talking on the phone, explaining that she is going to spend time in the spa before going to Chris Cavanaugh's speech. While she is in a jacuzzi, Lynette steals Meg's pass and stuffs her clothes in a bin. She arrives at the speech and is ushered to a seat in the front row. However, she is shocked when the person on stage announces that Meg is going to introduce Chris. She gets up on stage and admits that she isn't Meg, before making a cringe-worthy introductory speech. She is interrupted when Meg arrives in her dressing gown, shouting that Lynette stole her pass and her clothes. Lynette runs away. Back at home, Renee comes over and discovers that Tom and Lynette are in the middle of a fight. Tom yells at Lynette that she embarrassed him, adding that for years he took a back seat to her career but she can't do the same for him. When he storms off, Lynette tells Renee that the conference was awful because the plus ones were treated like second class citizens. Renee admits that she will just have to get used to it.
Carlos continues to ban Gaby from seeing Bree. Gaby and Bree stand in their gardens and speak on the phone. Bree admits that she can understand why Carlos feels the way he does and says that as much as she would like to see Gaby, she can't. Later, Bree goes to look after the Scavo house while they are away and Gaby arrives, claiming that she wanted to see Lynette. They start talking and eventually agree to have coffee together. Bree shuts the curtains so no-one can see them. Soon, they begin secretly spending time together. They admit that it is better because of the danger and Gaby suggests that they should go for a spa weekend. Later, Carlos arrives home and is surprised to see pineapple upside down cake - made by Bree - on the side. Gaby claims that she made it herself but Carlos is suspicious and asks her to make another one right now. He adds that he will watch her the entire time. Gaby goes to get the flour and spills some on herself. She tries to seduce Carlos, but he refuses to be distracted. Instead, she goes to clean off the flour and frantically calls Bree, asking for help. Bree decides to give her instructions on the phone and Gabrielle hides her headset with her hair. Bree guides her through the whole process as Carlos watches and makes her own cake at the same time. Later, the oven timer beeps and Gaby takes her cake out of the oven, but it collapses. She quickly throws a tea towel over it so that Carlos can't see and claims it needs to cool on the windowsill. As she distracts him, Bree rushes over and swaps her perfect cake with Gaby's disaster. Gaby tells Carlos that he should trust her and then shows him the perfect pineapple upside down cake. That weekend, she claims that she is going to the funeral of one of her old model friends. However, Carlos spots a red hair on her coat. Gaby claims that she hugged a clown at a birthday party, but Carlos takes her suitcase and discovers that she has packed bikinis and is planning a weekend away with Bree. He says that he banned her from seeing Bree and adds that ever since they moved to Wisteria Lane he feels like she always puts her friends first. He tells her to choose him or Bree, but Gaby tells him not to. However, he repeats that she has to choose.
Later, Gabrielle goes over to Bree's house, explaining that there has been a change of plan because Carlos knows about them. She asks if she can stay with Bree and Bree agrees - but is shocked when Gaby also ushers in her daughters.
Meanwhile, Karen is shocked when Felicia comes over. Felicia hands her a brooch that belonged to Martha, to thank her for keeping her secret for years. She adds that she will never tell anyone about the role that Karen played that night. Karen tells her it's not a good time to talk about it and is shocked to learn that Felicia is moving in next door. Inside, Karen asks Roy to get her a drink and has a flashback. She remembers seeing Felicia on the night that she cut off her fingers to frame Paul. Felicia explains what she has done and says that Paul will spend the rest of his life in prison if Karen says that she never saw Felicia. Karen is reluctant and begs Felicia not to make her do this, but eventually she agrees. Back in the present, Karen goes over to see Felicia, who explains that she got out of prison because her daughter died. Karen is shocked to hear that Felicia's daughter was Beth. Felicia claims that Paul wrote to Beth begging her to come and see him and made Beth fall in love with him. She alleges that when Paul was released he told Beth she didn't deserve to live and that he never loved her, so she killed herself. Karen is shocked and asks why Felicia wants to live on the same street as Paul. Felicia explains that she wants to make sure he never hurts another woman and Karen agrees to keep an eye on him as well.
Written by IngridPatriota on Feb 24, 2018


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text:
Q: How to integrate bessel function with variable bounds? In short I am trying to plot this function:
F(x)
which is an integration with a variable limit.
My code so far is:
import scipy
import scipy.integrate as integrate
import numpy as np
import matplotlib.pyplot as plt

X = np.linspace(0,6,1000)

def bessel(z): return scipy.special.kv(5/3,z)
def F(x): return x * scipy.integrate.quad(bessel(x),x,np.inf)

plt.loglog(X,F(X))

with an error that says "The truth value of an array with more than one element is ambiguous."
I've done this same integration in matlab, and the solution was to use "arrayfun" is there a similar function in python that applies F(x) to every element of X?


text:
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Editorial Review
MyFanPark Merges With Starsona Inc. To Create Leading Global Celebrity Engagement Platform
MyFanPark has announced its merger with Silicon Valley-based celebrity engagement platform, Starsona Inc. This transaction results in myFanPark entering the United States market – the company's fourth international market expansion this year – making it a leading global celebrity engagement platform, with a footprint across Africa, Europe, North America and the Indian subcontinent.
The amalgamation of the two companies comes on the back of a highly successful period for myFanPark which saw a 492% increase in the number of users on the platform and a 959% surge in total orders, with demand for certain talent increasing by 500%. As a result, the company saw its revenue climb 283%, which stimulated a range of new artists, athletes, entertainers, and influencers to join the platform around the world, and piqued Starsona Inc.'s interest in the business.
Joy Des Fountain, who will now serve as co-CEO alongside Peter Karpas, co-founder of Starsona Inc., said: "Our goal at myFanPark is to reimagine how people around the world are able to connect, engage, share with, and inspire each other. We can now offer an almost limitless range of ways for fans and celebrities from all over the world to forge authentic, highly personalised, and valuable relationships with each other."
She continues, "Celebrities registered on the new platform will now also have the ability to augment their fan and corporate engagements through a new range of individualised and unforgettable experiences. Going forward, in addition to shoutout videos, fans will be able to enjoy live calls, Q & A sessions, social media engagements, and even direct-message chats."
When asked what prompted the two companies to join forces, Des Fountain explains, "To deliver myFanPark's vision and international expansion plans, Starsona Inc. presented a natural fit, as it delivers best-in-class technology that enables never-before seen forms of engagement. However, more important than the combining of two businesses on paper, was establishing whether there was a natural synergy and cultural alignment between the people from two companies geographically located at different ends of the world, all whilst during a global pandemic and travel ban. From the first day that we met Peter and his team, it became clear that there was a real opportunity for our two businesses to significantly add to each other's strengths if we came together as one."
For Karpas, who brings decades of experience, having served as General Manager for North America Small & Medium Business at PayPal, Chief Marketing Officer at Intuit, and CEO of North America at Xero, "The growing desire for fans to engage more directly with celebrities represents a cultural shift and massive opportunity for our business and the talent registered on the platform. Our goal now is to further entrench ourselves in our regions through key partnerships and commercial opportunities that allow admired talent to create unique and authentic experiences for their fans or corporate clients: think career advice from business leaders, song lyrics from musicians, or coaching tips from world famous sporting heroes – now anything is possible."
As a result of the merger, fans can engage with more than 2,400 stars from around the world – from professional Nigerian footballer, Uchenna Kanu, and award-winning artists, Skales, IcePrince, and Daddy Andre; to South African Springbok, Faf de Klerk, and hip hop artist, Gigi LaMayne; to Indian Premier League superstar, Robin Uthappa; German football legend, Roman Weidenfeller; National Basketball Association MVP Kawhi Leonard, and even Beverly Hills 90210 actress, Tori Spelling.
The new platform won't be limited to individuals. The company is also looking to influential teams and brands to join its growing talent base. "Organisations wishing to promote and strengthen their association with talent registered on the platform will now be able to use myFanPark as a meeting place to boost their exposure to a combined audience of over 250 million authentic fans around the world."
According to Jean de Villiers, a Co-Founder of myFanPark, the company is also expanding its charity efforts. "With the partnership, we are adding to our 'Fans for Good' initiative by increasing our charity and fundraising capabilities. This means that, in addition to donating a portion of the proceeds from each paid-for interaction, the myFanPark platform will now let celebrities profile their own charities and create fundraisers for specific causes or organisations."
Celebrity myFanPark Starsona Inc.	2020-12-02
NewsProbe
Publisher's Corner
Let's End This Uncivil War, New US President, Joe Biden, Urges Americans
Everything We Do To Grow Economy, Change Lives Depends On Conducive Business Environment — Osinbajo
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Anambra Gov Election Holds Nov 6
History As Biden Takes Over From Trump Today
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US-Based Nigerian Professor, Odiraa Nwankwor, Selected To Work With UNN
Consider Malaria-Like Symptoms As COVID-19 Unless Until Proven Otherwise, Says Sanwo-Olu
Lifting 20 Million Nigerians Out Of Poverty In Next 2 Years Now Within Reach, Says Osinbajo
Nigerian, Obi Aginam, Joins United Nations University-CRIS
Alleged $5m Bribe To Malami: Akpabio Threatens Court Action
Traffic Violation: Lagos Task Force To Auction 88 Vehicles
Telcos Submit 43 Million NINs To NIMC For Verification
Soyinka Faults Quit Notice To Kukah, Says It's Unacceptable


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25/10/2012 - 16:14 | Analysis,News - Ivanishvili Confirmed as Prime Minister
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17/03/2012 - 19:23 | Analysis,News - Saakashvili: Talk of Civil War is 'Immoral' and 'Idiocy'
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Corridor Capital, LLC has partnered with management to recapitalize Nationwide Property & Appraisal Services, LLC ("Nationwide"), a national leader in real estate appraisal management services. EdgePoint led the negotiations of the sale and served as the exclusive financial advisor to Nationwide. Terms of the transaction were not disclosed.
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Corridor Capital, LLC's private equity strategy is to leverage its internal operating expertise and extensive network of executives to create value in control transactions in the lower middle market. Corridor, a dedicated fund, works actively in partnership with its portfolio company management teams to create sustainable and scalable infrastructure and to grow organically and through acquisition. The firm focuses on companies in specialty manufacturing, business services and environmental services. Corridor is headquartered in Los Angeles, California.


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