text:
\section{Introduction}

The advent of X-ray astronomy and the launch of Rossi X-Ray Timing Explorer (RXTE) since the last two decades
have significantly enhanced our understanding about the accretion processes
around compact sources, such as black holes (BHs) and neutron stars (NSs).
Most of these compact sources are in binaries, with the NS or the BH as the primary
which accretes matter from the companion star (secondary) either by Roche-lobe overflow or by capturing the
mass lost from the secondary in the form of winds.
Due to the presence of turbulent viscosity, a part of the gravitational potential energy
lost by the accreting matter is emitted in the form of radiations, chiefly in the soft X-ray domain. Even when
significant viscosity is absent, stored thermal energy is lost in X-ray domain by inverse Comptonization.
An outbursting Black Hole Candidate (BHC) primarily exhibits four different spectral states,
namely, hard state (HS), hard-intermediate state (HIMS), soft-
intermediate state (SIMS), and soft state (SS)
(e.g., McClintock \& Remillard, 2006; Nandi et al., 2012; Debnath et al., 2013).
Simultaneous analysis of the timing properties of these BHCs
reveal that low frequency Quasi-Periodic Oscillations (QPOs)
are also evident in the power density spectra (PDS) of these objects
(e.g., Remillard \& McClintock, 2006). Evolution of spectral and temporal
characteristics of several BHCs during their outbursts have been extensively
studied (e.g., McClintock \& Remillard, 2006; Nandi et al., 2012).
It has been noted that the various spectral states can be
related to different branches of the hardness intensity
diagram (HID; Belloni et al., 2005 and  Debnath et al., 2008) or, in a more
physical hysteresis diagram using accretion rate ratio and X-
ray intensity (ARRID; Mondal et al., 2014; Jana et al., 2016).
The HID or the ARRID shows the objects in different spectral states, generally, in the sequence: HS
$\rightarrow$ HIMS$\rightarrow$  SIMS$\rightarrow$  SS$\rightarrow$  SIMS $\rightarrow$ HIMS
$\rightarrow$ HS. It is well established that in order to interpret majority
of black hole spectra two types of spectral components, namely,
a multi-color blackbody component and a powerlaw component are needed.
The multi-color blackbody component seems to originate from an optically thick, geometrically thin Keplerian flow (Shakura \& Sunyaev, 1973)
while the powerlaw tail of the spectrum is believed to be emanated from
a ``Compton" cloud (Sunyaev \& Titarchuk, 1980, 1985).
Several theoretical and phenomenological models
ranging from a magnetic corona (Galeev et al., 1979) to a hot gas corona
over the disc (Haardt \& Maraschi, 1993; Zdziarski et al., 2003)
to a two component advective flow (TCAF) solution (Chakrabarti \& Titarchuk, 1995; hereafter CT95)
exist in the literature which attempts to explain the spectrum
and expound the nature and origin of this ``Compton" cloud.
In this paper, we use TCAF solution to investigate the spectral and timing properties of the source during its 2004 outburst.

The Galactic transient low mass BHXB H1743-322
is located at $\rm R. A.= 17^h46^m15^s.61$ and $\rm Dec = -32^o 14'00''.6$ (Gursky et al., 1978).
The discovery of this source goes back to August-September
1977, when Kaluzienski \& Holt (1977) reported its first X-ray activity with the Ariel V All
Sky Monitor. This was subsequently followed by observations from the HEAO I
satellite (Doxsey et al., 1977). Further activities of the source in the
X-ray band 12-180 keV were observed during the 1977-78 outbursts with the HEAO I
satellite (Cooke et al., 1984).
Based on the color-color diagram, obtained from the
spectral data of the HEAO I satellite, White \& Marshall
(1984) classified the source to be a potential BHC.
Since its first detection, it remained in the quiescent state till 1984 when
EXOSAT observations reported X-ray activities (Raynolds,
1999) which was subsequently followed by detection of activities by TTM/COMIS instruments on board MirKvant in 1996 (Emelyanov et al., 2000).
On March 21, 2003, the INTEGRAL
satellite detected a bright source named IGR J17464-3213 (Revnivtsev et al., 2003)
which displayed X-ray activities and later, RXTE confirmed the presence
of such an activity from the same region in the sky (Markwardt \&
Swank, 2003) validating the source to be H1743-322.
Since 2003, it exhibited several X-ray activities with quasi-regular intervals of about one to two years.
In order to investigate multi-wavelength properties of the source,
it was comprehensively monitored in X-rays (Parmar
et al., 2003; Remillard et al., 2006;
McClintock et al., 2009), IR (Steeghs et al., 2003), and in
radio bands (Rupen et al., 2003) during its 2003 outburst.
McClintock et al. (2009) and Miller-Jones et al. (2012) eventually followed up
further investigations of the source in the multi-wavelength
during its 2003 and 2009 outbursts respectively.

The mass of the BHC in H1743-322 has not yet been dynamically measured, although several attempts have been made
to predict the mass of the BH. Analysing 2003 outburst data, Shaposhnikov \& Titarchuk (2009, ST09) calculated mass of this black hole candidate
to be $13.3\pm3.2$ $M_\odot$ using their QPO frequency-Photon Index correlation method.
McClintock et al. (2009) estimated its mass to be $ \sim 11 M_\odot$ using their high frequency QPO correlation method.
From the model of high frequency QPOs based on the mass-angular momentum (i.e., spin of the black hole), P\'{e}tri (2008) predicted that its mass should lie in the range of $9-13 M_{\odot}$.
Based on its spectral and timing properties using two recent outbursts (Molla et al. 2016a, hereafter M16a)
estimated the mass of the BHC to be $M_{BH}=11.21^{+1.65}_{-1.96}$. These authors also used the method of ST09 and narrowed down the range to $11.65\pm0.67M_{\odot}$.
The source is reported to be at a distance of $\rm 8.5 \pm 0.8$ kpc with the
inclination angle of $\theta \sim 75^o \pm 3^o$.
Steiner et al. (2012) also constrains to the spin $a$ of the source,
$-0.3 < a < 0.7$ with a 90\% confidence level.

Recent outbursts of H1743-322 in 2010 and 2011 again showed the characteristic
state transitions (Shaposhnikov and Tomsick, 2010; Shaposhnikov, 2010) as observed in other outburst sources (Nandi et al., 2012).  It was pointed out by Debnath et al. (2010) that depending upon the outburst light
curve profiles, there are mainly two types of outbursting
BHCs: the `fast-rise slow-decay' (FRSD) type and the `slow-rise slow-decay' (SRSD) type. The source H1743-322 belongs to the first category.
Debnath et al. (2013) investigated the average temporal and spectral properties of the object
using  combined disc black body (DBB) and power law (PL) model using data of 2010 and 2011 outbursts.
Mondal et al. (2014) analysed the RXTE/PCA data during its 2010 outburst using the TCAF
solution allowing the normalization $N$ of the TCAF model to vary in order to get the best fit. On the other hand, M16a analysed
the data of H1743-322 using TCAF solution during its 2010 and 2011 outbursts, restricting
the normalization $N$ within a narrow range to estimate the mass of the central object.
Here, we follow the same procedure of M16a and M16b to analyse the 2004 outburst of H1743-322
which not only enables us to understand the underlying accretion flow dynamics but also allows us to give a fresh
estimate to the mass of the BHC H1743-322. We first determine the average value of normalization by keeping it free within a narrow range. The constant, averaged value of the normalization is then used to refit the spectral data and estimate the mass of the BHC. The 2008b outburst was a `failed outburst' and hence was not analysed.
The 2005 outburst could not be analysed due to lack of data (Coriat et al. 2011). The outburst in 2003 had significant
radio activity, which is currently being analysed by Nagarkoti et al. (in preparation). From the rest of the cases,
2004 outburst was the most prominent one, in terms of total flux and duration.
Hence, we selected this 117 day long 2004 outburst for our analysis.

Since several outbursts have already been studied one could surmise that analysis of yet another outburst would be of limited use.
If one observed the sequence of outbursts, the one in 2003 took place after about twenty years and after that
there are quasi-regular outbursts, some very small and some moderate. The one in 2003 is very anomalous in the sense that its
intensity was more than five times larger than the next prominent ones, such as those in 2004, 2010, 2011 etc.
and at least 10 to 15 times stronger than several others. This is probably an indication that 2003 outburst could have been triggered by a
non-linear instability and the system is slowly settling and relaxing after subsequent outbursts, probably before going to a long quiescence state again. It is thus no surprise that ST09 estimation of mass of 2003 outburst had a huge error margin while M16a estimate using the same method but 2010 and 2011 data shows a narrower margin. Assuming 2003 outburst is truly anomalous, the first stereotypical outburst is in 2004 and it is important to study this. While fitting the spectra we find that it is highly soft
in much of the time where a standard disk is enough to fit the data.
The region where both spectral components are seen prominently, and both the flow components are
important is in the declining state. So we concentrate only on the declining state of 2004 data.

Judging from the fact that in initial outbursts, the source was going
to very bright soft states and then more relative times have been spent in harder states,
every outburst can be thought to be separately important and combination of the evolution of physical parameters
may lead to the understanding of the long term behaviour of the system. Furthermore, from the light curves
it is easy to see that decay time scales and peak fluxes are different and both of these parameters are
governed by viscosity in the Keplerian flow. The pattern of mass accretion rate
variations are also found to be different from one outburst to the other. Even the accuracy of the estimated mass is vastly different for the same method (M16a).
Thus it is essential that every outburst be studied as accurately as possible.

We organize the paper in the following way: In \S 2 we discuss the salient features of the TCAF solution
and the Propagatory Oscillatory Shock (POS) model.
In \S 3, we discuss observation and methods of data analysis implementing
HEASARC's HEASoft software package. In \S 4, we present the results obtained from the spectral analysis using the
TCAF solution and the POS model. Finally, in \S 5 we conclude with a brief discussion summarizing our main findings with some remarks for future work.

\section{Method of Analysis}

\subsection{Two Component Advective Flow (TCAF) Solution}

Prior to the launch of RXTE, Chakrabarti \& Titarchuk (CT95) explored the well-established solution of a transonic flow (see,
Chakrabarti, 1990, Chakrabarti 1996, hereafter C96) and proposed that the accretion flow generally exhibits a two-component behavior,
namely, a viscous Keplerian flow sandwiched by a weakly viscous sub-Keplerian flow (Fig. 1).
This solution, popularly known as the Two-Component Advective Flow (TCAF) solution in the literature enunciates that the sub-Keplerian
halo component, envelops the Keplerian disc and since it requires negligible viscosity to accrete, falls into the BH with a much higher
radial velocity (Soria et al., 2001; Smith et al., 2002; Wu et al., 2002; Cambier \& Smith, 2013; Tomsick et al., 2014).
The sub-Keplerian flow is advective, can reach supersonic speeds and has angular momentum less than that of a Keplerian distribution.
Hence, it undergoes a centrifugal pressure supported
shock transition to become subsonic in between the two sonic points. The complete solutions are worked out in detail in
Chakrabarti, 1989 (hereafter C89), and C96.
The centrifugal pressure impedes the flow and as a result a standing or oscillating shock is formed depending on whether the
Rankine-Hugoniot conditions are satisfied (C89, C96). Thus, the flow puffs up in the vertical direction, and forms the CENtrifugal
pressure dominated BOundary Layer (CENBOL). This CENBOL acts as the Comptonizing cloud which up-scatters the seed black body photons
coming from the Keplerian disc.
In the natural hard state of a BHC, this is the only component that is present.
The component near the equatorial plane has a viscosity higher than the critical value and is Keplerian in nature
having the characteristics of a standard disk. This component is not always present close to the black hole. When the outburst is triggered
by increase of matter and viscosity, this disk formation is initiated from outside and it moves in on a daily basis, increasing the
supply of Keplerian matter as well as soft seed photons which are intercepted by the CENBOL and are inverse-Comptonized through repeated
scattering. A typical route of the photon emerging from the Keplerian disc to the observer via CENBOL is shown in Fig. 1.
Initially the hard state is formed when the rates were still low and shock front was hundreds of Schwarzschild radii away and the
advective (halo) component rate increases first due to its short infall time. Subsequently, the Keplerian rate starts to increase since its
angular momentum is high and it is to be transported by viscosity. Here the object goes to hard intermediate states. The rate continues to rise
and the cooling time scale inside CENBOL starts to be smaller compared to the infall time scale when the condition of oscillation of the
shock front is violated and the QPO seen thus far, becomes sporadic and state becomes soft-intermediate. Finally, if Keplerian matter supply is really high, and the viscosity can transport angular momentum very efficiently, soft photons overwhelmingly cools the CENBOL removing it
altogether and the soft state is produced. This gradual transformation of the size and shape of the CENBOL is clearly depicted
in Fig. 2. When the companion turns off the active phase, the process is reversed albeit in a different time scale.
Thus, by giving a clear theoretical origin of the Compton cloud (CENBOL) and
self-consistently amalgamating the synergy and the inter-conversion of the two components through
viscosity, the TCAF solution provides a clear picture of the entire outburst process and obviates the need of phenomenological
models in the subject.

For the calculations, all the equations are reduced to their dimensionless forms. The important references can be found in Chakrabarti 1989 (hydrodynamical equations), CT95 (spectral, radiative transfer equations), Debnath et al. (2015a). The last one is the first paper after inclusion of TCAF in XSPEC, where important equations (eq. no. 1 to 5) of TCAF solutions are summarised.

Lengths are measured in units of
$r_S=2GM_{BH}/c^2$ ($G$ and $c$ being gravitational constant and the velocity of light),
and the accretion rates are measured in units of Eddington rate
(also a function of the black hole mass $M_{BH}$). The disc accretion rate ($\dot{m_d}$),
the halo accretion rate ($\dot{m_h}$), the shock location ($X_s$), the shock compression ratio ($R$) and the mass of the BHC ($M_{BH}$)
are taken as input parameters and a resulting spectrum is generated. The first four parameters are dependent on the flow properties.
Hence, their time-variation reveals the accretion flow dynamics around the object during an outburst.
Numerical simulations (Giri \& Chakrabarti 2013)  and spectral studies (Ghosh et. al. 2011) of BHCs reveal that the TCAF solution
is the most general solution for accreting matter onto a black hole. Self-consistency and stability check of the transonic solution by
Giri \& Chakrabarti (2013) and Mondal \& Chakrabarti (2013) corroborates that an advective flow will eventually give rise to a TCAF
solution (CT95) when viscous stress near the equatorial plane is substantial. This solution therefore invokes two types of energy
extraction processes into  a single coherent framework: i) viscous dissipation in the Keplerian component to produce soft X-rays and ii) Inverse Comptonization of these soft photons to produce hard photons by stored thermal energy in the weakly viscous CENBOL.

\begin{figure}
  \centering
\includegraphics[height=7.5cm,width=15.0cm]{figure1.eps}
\vskip-0.5cm
\caption{A schematic diagram of the accretion flow dynamics and radiation processes in a Two Component
Advective Flow (TCAF) solution. Adapted from CT95.}
\label{lc}
\end{figure}

After obtaining the shape of the overall spectra, suitable model normalization $N$ is used to raise or lower it to match
the observed spectra. In diskbb plus powerlaw model, the normalization comes only from the disc
integrated photon number which is used to obtain the inner edge of the truncated disc.
In TCAF fits, one cannot separate the black body and powerlaw components since the disc
radiation and its Comptonized spectrum are summed up along with the reflected components in the fits file. The information about
the inner edge of the truncated disc is in determining the shock location which is also the outer edge of the Compton cloud (CENBOL).
Since these information are already fed into the grid of the fits file, we only require a constant normalization which is primarily
mass ($M_{BH}$), distance (D in units of $10$ kpc) and inclination angle
(i) dependent through a functional relation $N \sim [r_S^2/4 \pi D^2] sin(i)$ (Molla et al. 2016b, hereafter M16b). Error in mass determination would give rise to
error in normalization. Ideally if the CENBOL was lying in a plane, the
inclination angle would be globally constant, unless the disc is precessing (which we do not assume here).
Also, $M_{BH}$ should not vary over the time scales of observation. Since $M_{BH}\sim T^4$, and the spectral fits are sensitive
to the temperature $T$, a small error in determination of $T$ gives rise to a significant error in $M_{BH}$. This in turn is
reflected in the normalization. Moreover, there can be changes in the peak flux with spectral states when the CENBOL
changes its shape and size self-consistently. The variation of flux is due to the variation of accretion rates
($\dot{m_d}~and~\dot{m_h}$), shock location ($X_s$) and compression ratio ($R$). In any case, our result is independent of
the exact value of normalization, and our requirement is that it may remain in a narrow range so that we are certain
the fitting routine stays in the same global minimum. The average value,
for statistical reasons, is taken as the constant value of normalization for the outburst and the entire study is repeated with
this constant normalization. Under this assumption, if the $M_{BH}$ fluctuates, $D$ and $i$ have to adjust to ensure a constant $N$,
though that does not affect our analysis. For all practical purposes, this $N$ is `fixed' from one outburst to the other as it should be
when precession of the disc is absent.

Recently, the TCAF model (CT95; Chakrabarti, 1997) has been successfully incorporated in HEASARC's spectral analysis
software package XSPEC (Arnaud, 1996) as a local additive table model (Debnath, Chakrabarti \& Mondal 2014;
Mondal, Debnath \& Chakrabarti 2014; Debnath, Mondal \& Chakrabarti 2015a; Debnath, Molla, Chakrabarti \& Mondal 2015b;
Jana et al. 2016; Chatterjee et al. 2016; Mondal, Chakrabarti \& Debnath 2016; M16b).
It accomplishes fitting of the spectral data of several transient BHCs
(e.g., H 1743-322, GX 339-4, MAXI J1659-152, MAXI J1836-194), during their X-ray outbursts which in turn
enables us to get a much clearer picture of the accretion flow dynamics in terms of the disc and halo mass accretion rates,
the location and size of the Comptonizing cloud (here, CENBOL) and the strength of the shock, which in conjunction with
the size and halo rate gives an idea of the optical depth.

 \begin{figure}
  \centering
\includegraphics[height=7.5cm,width=15.0cm]{figure2.eps}
\vskip-0.5cm
\caption{A schematic diagram showing the evolution of the CENBOL and the Keplerian disc in a Two Component Advective Flow (TCAF)
solution. At the onset of an outburst, the halo is dominant and the shock front is far away (hard state: HS).
The Keplerian component moves inward, cooling the CENBOL and making it smaller (hard intermediate:HIMS). For high disc accretion rate, first the
CENBOL cools and QPOs became sporadic (soft Intermediate state: SIMS) and finally the halo component is
cooled down totally (soft state: SS). The reverse sequence follows when the supply at the outer edge halted.
Adapted from Chakrabarti (2016).}
\label{lc}
\end{figure}

\subsection{Propagatory Oscillatory Shock (POS) model}
Once the Keplerian disc is formed, the CENBOL is cooled down gradually.
If the cooling timescale of the CENBOL lies within $\sim 50\%$ of the infall time scale from the shock front to the black hole,
a resonance occurs when the shock or the outer edge of the Compton cloud starts to oscillate (Molteni, Sponholz \& Chakrabarti, 1996;
Chakrabarti \& Manickam, 2000; Chakrabarti et al. 2015). The oscillation of the shock front leads to the generation of low frequency
quasi-periodic oscillations (QPOs) in the power density spectra of the light curves. Due to variation of shock conditions with the
changes in disc and halo accretion rates, the average shock location moves inward (outward) for the rising (declining)
phase of the outburst (Fig. 2). Simultaneously, the QPO frequencies evolve as well.

The frequency of oscillation of the shock front, which in turn is related to the QPO frequency ($\nu_{qpo}$) is obtained
from the inverse of the infall time ($t_{infall}$). If, $c$ is the speed of light, $G$ is the gravitational constant and $M_{BH}$
is the mass of the black hole, then the unit of frequency is given by,
$\nu_{s0}=\frac{c^3}{2GM_{BH}}$. The QPO frequency is then written as,
\begin{center}
$\nu_{qpo}=\nu_{s0}/t_{infall}=\frac{c^3}{2GM_{BH}}\frac{1}{[RX_s(X_s-1)^{1/2}]}$
\end{center}
where, $R$ is the shock compression ratio and $X_s$ is the shock location in units of $r_S$ (Chakrabarti et al. 2008;
Chakrabarti et al. 2009; Debnath et al. 2010; Nandi et al. 2012; Debnath et al. 2013).
\\
According to the POS model, the shock location varies with time as,
\begin{center}
$X_s(t)=X_s(0)\pm tv_0/r_S$,
\end{center}
where $v_0$ and $X_s(0)$ are the initial location and velocity of the shock. The plus (minus) sign is associated with the shock front
for declining (rising) phase. This can, in turn, be used to determine the mean radial velocity of the shock front during the outburst
which further enables us to study the evolution of $X_s$ and hence the evolution of the QPO frequencies.
The POS model has a parametric dependence on the mass $M_{BH}$. Hence, if QPOs are observed in a series of consecutive days,
then the POS model can be used to fit the variation of the QPO frequency with time.
The value of mass which gives the best fit to the data will be the mass of the BH.

\section{Observation and Data Analysis}

RXTE/PCA covered the 2004 outburst of H1743-322 spanning from July 11, 2004 (MJD=53197.287) to November 5, 2004 (MJD=53314.749).
42 observations were recorded by RXTE during the aforementioned period with an average gap of $\sim$ 3 days between consecutive
observations. We use HEASARC's software package HEASoft, version HEADAS 6.18 and XSPEC version 12.9.0 to carry out our data
analysis procedure. In order to generate the source and the background ``.pha" files and fit the spectrum exploiting the
TCAF solution we follow the procedure adopted by Debnath et al. (2013, 2014). For spectral analysis, the Standard2 mode
Science Data of PCA (FS4a*.gz) were used. Spectra from all the Xenon layers of PCU2 consisting of 128 channels (without
any binning/grouping of the channels) were extracted for all the observational IDs. Dead-time and pca breakdown correction
were incorporated in our analysis. We extracted the PCA background by applying the command ``runpcabackest" and by using
the latest bright-source background model. In order to take care of the South Atlantic Anomaly (SAA) data we incorporated
the pca saa history file. The task ``pcarsp" was used to create the response files.
For preparing the power density spectra (PDS) all active PCUs were used for a broad energy binned between 0-35 channel data.
The 2.5 - 25 keV PCA spectra of these observation IDs with appropriate background subtraction were fitted with TCAF solution
based additive model fits file. To accomplish the best fit, a Gaussian line was used to model the iron line emission.
Throughout the outburst, the hydrogen column density ($N_H$) was kept fixed at $1.6 \times {10^{22}}$ atoms $\rm cm^{-2}$
(Capitanio et al. 2009) for absorption model \textit{wabs}. A systematic instrumental error of $1\%$ was assumed. We used
``err" command to find out $90\%$ confidence error values in model fitted parameters.

Here we initially fit the entire 117 day long outburst using wabs*(diskbb+PL) model. Next, we fit the last $27$ days
of the outburst (declining phase) by keeping $\dot{m}_d$, $\dot{m}_h$, $X_s$, and $M_{\rm BH}$ free and normalization within
the range $10<N<20$ as in Molla et al. (M16a). Next, using the POS model, the velocity of the shock front was found out using
the parameters as obtained from the previous analysis. The same process of spectral fits using the TCAF model was repeated
using the average value of normalization obtained from the previous analysis. For this purpose, the model fits file
(TCAF.fits) was used which uses the theoretical spectra-generating software by varying the five basic input parameters
in the suitably upgraded CT95 code and is then incorporated in the XSPEC as a local additive model. The version of TCAF
used for fitting the spectra in the present work is TCAFv0.1.R3.fits used in Debnath et al. (2015a) and
references therein.

\begin{figure}
  \centering
\includegraphics[scale=0.7]{figure3.eps}
\caption{Variation of (a) the \textit{diskbb} Temperature ($\rm T_{in}$) in units of keV,
(b) the \textit{power law} photon index ($\Gamma$),
(c) the \textit{diskbb}
flux ($\rm Flux_{diskbb}$) in units of $10^{-9}$ ergs $\rm cm^{-2} s^{-1}$,
(d) the \textit{powerlaw}
flux ($\rm Flux_{PL}$) in units of $10^{-9}$ ergs $\rm cm^{-2} s^{-1}$,
(e) the total flux ($\rm Flux_{Total}$) in units of $10^{-9}$ ergs $\rm cm^{-2} s^{-1}$,
(f) the ratio of \textit{diskbb} flux ($\rm Flux_{diskbb}$) and \textit{powerlaw} flux ($\rm Flux_{PL}$) $\rm, Ratio_{flux}$, and
(g) the inner edge of the disc ($\rm R_{in}$) in units of km, given by the
diskbb normalization with MJD (days).
All the above variations are in the 2.5-25 keV energy band. The declining phase, that was fitted with TCAF solution, is shaded with yellow (colour online).}
\label{fit0}
\end{figure}

\section{Results}

In this Section, we present the results obtained from the analysis of the data of H1743-322 during the 2004 outburst by the TCAF fits.

A comparison of RXTE/ASM light curves of H1743-322 between 2003 and 2009 shows that the source predominantly resided
in the softer states during the 2004 outburst, namely, soft-state (SS) and soft-intermediate state (SIMS), and only towards
the end of the outburst the source entered in the hard-intermediate state (HIMS) and hard-state (HS) (Fig. \ref{fit0}(e)).
Capitanio et. al (2005) also reports a similar behavior of the source during this outburst.

Figures \ref{fit0}(a) and \ref{fit0}(b), illustrate variation of \textit{diskbb} temperature $\rm T_{in}$ and the \textit{powerlaw}
photon index $\Gamma$ with MJD. Figures \ref{fit0}(c) and \ref{fit0}(d) show the variation of the flux
contributed by \textit{diskbb} and \textit{powerlaw}
models respectively, while Fig. \ref{fit0}(e) shows the variation of the total spectral flux. The ratio of \textit{diskbb} flux ($\rm Flux_{diskbb}$) and \textit{powerlaw} flux ($\rm Flux_{PL}$), $\rm(Ratio_{flux}$) is shown in the panel \ref{fit0}(f).
The variation of the inner edge of the disc ($\rm R_{in}$), given by the
diskbb normalization with MJD is shown in Fig. \ref{fit0}(g).
We calculated the individual flux
contributions for the \textit{diskbb} and the \textit{powerlaw} components
by using the convolution model ``cflux" once for the \textit{diskbb} and then for the \textit{powerlaw},
to fit the spectra in the 2.5-25 keV energy band.
The analysis with \textit{wabs*(diskbb+powerlaw)} model also reveals that the data for the rising phase was only
obtained well after the object settled into Soft-Intermediate state. Subsequently, during the rising phase, the peak and
the initial part of the declining phase of the outburst the underlying accretion flow was primarily governed by a single
component, i.e., the Keplerian flow. As a result, its spectrum is principally fitted by \textit{diskbb} and the additional
advective component is not needed. Since in TCAF we are interested to study the interplay between the two components,
we concentrate on the declining phase during MJD=53287.484 - MJD=53314.749 period.

\subsection{Spectral Data Fitted by TCAF model}
Table \ref{table:tcaf1} illustrates the variation of the physical parameters, namely, the disc accretion rate ($\dot{m}_d$),
the halo rate ($\dot{m}_h$), the shock location ($X_s$) which gives an indication of the size of the Compton cloud and
the strength of the shock ($R$) with days (MJD) in the 2.5-25 keV (3-53 channels) energy band during the declining phase
of the outburst. To explicitly show that the rates are independent, we also plot the ratio ARR(=$\dot{m}_h$/$\dot{m}_d$). The model normalization ($N$) is kept in the range $10-20$. The average value of $N$ ($N_{avg}$) is
determined and the same procedure is repeated for the constant value of $N=N_{avg}=13.65$,  which we think is a good estimate of the normalization. If we ignore possible precession in the system, contribution from jets which have not been introduced in TCAF, and the possible change in shape with states, this can be treated as true normalization for the system.
The spectral evolution of the rest of the parameters are shown in Table \ref{table:tcaf2}.
The trends of variation of the flow parameters were found to be similar in both cases. Hence, we only discuss the spectral evolution for $N$ in the range $10-20$.

\textbf{Spectral Evolution of the Declining Phase and Corresponding TCAF Parameters:}

(i) \textit{Hard-Intermediate State (HIMS)}: For a period of $\sim 13$ days, MJD=53287.484 to
MJD=53300.208, the object seems to have remained in the Hard-Intermediate state (HIMS) which is evident from
Table \ref{table:tcaf1} and Fig. \ref{fit1}. During this period the PCA flux consistently
decreases as long as $\dot{m}_d$ is greater than $\dot{m}_h$, from MJD=53287.484 to MJD=53293.882
and then remains roughly constant (Fig. \ref{fit1} a). On MJD=53296.834, $\dot{m}_h$ becomes greater
than $\dot{m}_d$ and shock suddenly moves outward from $X_s=27.803 r_S$ to $X_s=75.662 r_S$. During the HIMS
to HS transition, on MJD=53296.834 and MJD=53300.208, QPOs were observed in the power density spectra (PDS).
A typical spectra of this state, along with the unfolded models and residue is shown in Fig. \ref{fitspec2}(a).

(ii) \textit{Hard-state (HS)}: From the data in Table \ref{table:tcaf1} it seems after MJD=53300.208 the source entered
in the Hard-State (HS) and remained there till the end of the observation. A typical spectra of this state, along with
the unfolded models and residue is shown in Fig. \ref{fitspec2}b. The PCA flux also went down from this day and
remained low till the end of the observation which is characteristic of the Hard State. This is evident from Fig. \ref{fit1}a.
No QPOs were observed in the power-density spectrum of the source during these days.
The disc accretion rate which had fallen towards the end of the Hard Intermediate State (HIMS) remains low ($\sim 0.022$)
while the halo rate remains comparatively higher ($\sim 0.13$). The shock front moves further and further outward with time,
from $\sim 75~ r_S$ to $\sim 171~ r_S$, in a period of $\sim 14~ \rm days$. The propagation of the shock front not only gives
the clear picture as promised by the TCAF spectral fits, but also helps us to use another method of verifying the mass of the
object by an independent method, namely, by the use of Propagatory Oscillatory Shock(POS) model (Chakrabarti et al., 2005, 2008;
Debnath et al. 2010, 2013; Nandi et al. 2012). The spectral analysis restrict both mass and normalization in a narrow domain.
We investigate below to check whether the same mass range is obtained from the timing analysis or not.

The mass was determined to be $\langle M_{BH} \rangle=12.36\pm 1.73~M_{\odot}$, with an average $\langle \chi^2_{red} \rangle = 0.82 \pm 0.20$, and the average normalization is found to be $N_{avg}=13.65\pm 2.49$. The same process, when repeated by using a fixed $N=N_{avg}=13.65$, yielded similar results. These are shown in Fig. \ref{fit2}.
The mass was determined to be $\langle M_{BH} \rangle=12.19\pm 1.88~M_{\odot}$, with an average $\langle \chi^2_{red} \rangle = 0.79 \pm 0.19$.
The peak of the Gaussian line profile was close to the same value as that of the previous case.

\subsection{Correlating spectral and timing properties}

Timing analysis was limited by the lack of observable low-frequency QPOs in the declining phase of the outburst. Out of the 14 data IDs, only 2 days showed prominent QPOs. We use this to determine the mass of the object separately.
We use the POS model in determining the QPO frequencies from the spectral fit parameters, and use the same equations to obtain
the value of mass, for which the deviation between the theoretical and observational QPO frequencies are minimum. We also
determine inward velocity of the shock front for the first day of QPO observation to compare our results with previous works
(Chakrabarti \& Manickam, 2000; Chakrabarti et al. 2009; Debnath et al. 2013).

Each PDS was analysed with a Lorentzian fit using the ftools commands. The values of the centroid frequency, full-width at
half-maxima and peak power are obtained with 90\% confidence. From the values of $X_s,\ R,\ M_{BH}$, the oscillation frequency
of the shock front which is directly related to the frequency of the QPOs can be derived and compared to the frequency obtained
independently from the analysis of the power density spectrum, $\nu_{QPO}^{PDS}$.

The QPO frequencies obtained from the POS model using the corresponding values of the TCAF parameters taken from Table 1,
along with their respective systematic errors are given in Table 3, and is denoted by $\nu_{qpo}^{POS}$. The same calculation is
repeated for the case with constant normalization, using the respective parameters from Table 2 and is reported in Table $4$.
We found that these two values agree with each other within the error bars.

Next, on MJD=53296.834 and MJD=53300.208, when QPOs were observed, we used the corresponding fit parameters $X_s$ and R
and varied the mass from 9 to 15 $M_{\odot}$ to calculate the corresponding QPO frequencies, $\nu_{QPO}$.
The chi-square of the distribution is calculated using $\nu_{QPO}^{PDS}$. The value of the mass for which the chi-square is
minimum corresponds to $M_{BH}^{POS}$ which is quite close to the value of the mass obtained from the TCAF fits, $M_{BH}$,
on each of the days.

We calculated the velocity of the shock front for the first day (MJD=53296) of QPO observation. The velocity of the
shock front is $v_0=107.0_{-18.083}^{+18.083}~cm s^{-1}$, which is of the order of values found by Debnath et al. (2013).
For the constant normalization case, it came out to be $v_0=31.6_{-16.146}^{+16.146}~cm s^{-1}$. This is in the same ball park
for all the outburst sources GRO J1655-40 (Chakrabarti et al., 2005, 2008), XTE J1550-564 (Chakrabarti et al., 2009),
GX 339-4 (Debnath et al., 2010; Nandi et al., 2012), H 1743-322 (Debnath et al., 2013) and IGR J17091-3624 (Iyer et al., 2015)
and is generally thought to be due to the change of pressure in CENBOL due to Compton cooling which drives the shock
radially (Mondal et al. 2015). The deviation between these two approach may be due to the fact that POS had only two points to fit the evolution of QPOs. With constant normalization, the position of the shock front does not change
much during the two consecutive days which gives rise to a large systematic error in its measurement which is responsible
for the discrepancy between the shock velocities in the two cases.

\begin{figure}
  \centering
\includegraphics[scale=0.8]{figure4.eps}
\caption{Variation of (a) the total PCA flux (in units of $\rm 10^{-9}$ ergs $\rm cm^{-2} s^{-1})$,
(b) the disc accretion rate $\dot{m}_d$ (in Eddington units),
(c) the sub-Keplerian halo accretion rate  $\dot{m}_h$ (in Eddington units) ,
(d) the accretion rate ratio, ARR($=\dot{m}_h/\dot{m}_d$),
(e) the mass of the black hole (in units of $M_{\odot}$),
(f) the shock location $X_s$ (in units of $r_S$),
(g) the shock strength $R$, and
(h) the normalization of the TCAF model, with day (MJD).
Note that the normalization is restricted between $10-20$ in the above fits.
Variation of all the aforementioned quantities are studied in the 2.5-25 keV energy band.
We have added error-bars corresponding to Fig. \ref{fit1}(c) and Fig. \ref{fit1}(e). The remaining
error-bars are too inconspicuous to be marked.
}
\label{fit1}
\end{figure}
\begin{figure}
  \centering
  \includegraphics[height=7.5cm,width=7.0cm,angle=-90]{figure5a.eps}
\includegraphics[height=7.5cm,width=7.0cm,angle=-90]{figure5b.eps}
\vskip-0.0cm
\caption{Unfolded spectra with residue of two observations (ID: 90115-01-03-00 (a) and 90115-01-06-00 (b)) for energy 2.5-25.0 keV,
fitted with \textit{wabs(TCAF+Gaussian)} models.}
\label{fitspec2}
\end{figure}

\begin{figure}
  \centering
\includegraphics[scale=0.8]{figure6.eps}
\caption{Variation of
(a) the disc accretion rate $\dot{m}_d$ (in Eddington units),
(b) the sub-Keplerian halo accretion rate $\dot{m}_h$ (in Eddington units),
(c) the accretion rate ratio, ARR($=\dot{m}_h/\dot{m}_d$),
(d) the mass of the black hole (in units of $M_{\odot}$),
(e) the shock location $X_s$ (in units of $r_S$),
(f) the shock strength $R$, with day (MJD)
Variation of all the aforementioned quantities are studied in the 2.5-25 keV energy band keeping the
the normalization of the TCAF model fixed to $N=N_{avg}=13.65$.
We have added error-bars corresponding to Fig. \ref{fit2}(b) and Fig. \ref{fit2}(d). The remaining
error-bars are too inconspicuous to be marked.
}
\label{fit2}
\end{figure}

\subsection{Mass estimation using TCAF and POS model fits}

The three different methods used in determining the mass of the black hole, yield masses in the same range, upto the corresponding error-bars. We obtain the average value of mass to be $\langle M_{BH} \rangle=12.36\pm 1.73~M_{\odot}$, for spectral fits with free normalization. The average value of mass is found to be $12.19 \pm 1.88~M_{\odot}$, when the normalization is kept constant at $N=N_{avg}=13.65$. The POS model was applied to both the scenarios for both the observation IDs. In the first case, the masses obtained were $14.011~M_{\odot}$ and $10.479~M_{\odot}$ respectively. For the second case, the masses were $12.156~M_{\odot}$ and $11.125~M_{\odot}$ respectively. All four of these values lie within the range estimated by the spectral fits with constant normalization ($10.31~M_{\odot}-14.07~M_{\odot}$). Incidentally, Molla et al. (M16a) also obtained the average value of normalization $N\sim 15.55$ which lies within the range predicted
by us. Our result conforms with the previous predictions of Shaposhnikov \& Titarchuk (2009) and McClintock et al. (2009).
However, both these methods use mass of other BHC as a reference to calculate mass of an unknown BH, but our method gives
an independent method, where mass can be estimated even from one spectral fit using TCAF solution. We do not require to
know the mass of other BHCs to estimate mass of an unknown BHC. In Shaposhnikov \& Titarchuk 2009, mass only can be predicted
if there are sufficient observations in the transition and saturation branches of their QPO frequency-Photon Index correlation
plot. Similarly, in high frequency correlation method (used in McClintock et al. 2009), mass of those unknown BHCs can be
predicted, which have shown signature of HFQPOs (so far only 7 BHCs). These sources have shown multiple set (2:3) of HFQPOs.

The iron line emission profile was found to be peaked at around $6.5$ keV for all the fits, with an
average of $6.57 \pm 0.13$ keV. Fig. \ref{fit1} shows variations of all the TCAF parameters with MJD.
Thus, we find that the normalization $N$ of the TCAF model does not change over a period of seven years
i.e., from 2004-2011 indicating that probably the accretion disc is not precessing with significant amplitude.

\begin{table}
\tiny
\vskip0.2cm
{\centerline{\large Table \ref{table:tcaf1}}}
\caption{
TCAF Model Fitted Parameters in 2.5-25 keV energy band for normalization in the range $10-20$. Here, we list the variations
of disc accretion rate ($\dot{m_d}$) and halo accretion rate ($\dot{m_h}$) in Eddington units, shock location ($X_s$) in
Schwarzschild radius, shock compression ratio ($R$), mass of the BHC ($M_{BH}$) in $M_{\odot}$ and model normalization ($N$)
with MJD along with their errors.
The reduced ($\chi^2$) values for each case is also shown in the last column.}
{\centerline{}}
\begin{center}
\begin{tabular}{c c c c c c c c c c}
\hline
\hline
$\rm Obs. $ & $ \rm Id. $ & $\rm MJD $ & $ \rm \dot{m}_d ~(\dot{M}_{Edd})$ & $ \dot{m}_h~(\dot{M}_{Edd}) $ & $ X_s~(r_S) $ & $ R $ & $ M_{BH}~(M_{\odot}) $ & $ N $ & $\chi^2/dof$ \\
\hline
$\rm 1$ & $\rm X-02-00$ & $\rm 53287.484$ & $ \rm 0.785^{+0.108}_{-0.028}$ & $\rm 0.070^{+0.017}_{-0.001} $ & $\rm 29.790^{+0.019}_{-0.019}$ & $ 1.070^{0+0.001}_{-0.001}$ & $\rm 13.774^{+0.143}_{-0.141}$ & $ \rm 19.496^{+0.165}_{-0.164} $ & $ \rm 37.41/40 $ \\
$\rm 2$ & $\rm X-02-01$ & $\rm 53290.036$ & $ \rm 0.649^{+0.007}_{-0.007}$ & $\rm 0.064^{+0.001}_{-0.001} $ & $\rm 28.862^{+0.023}_{-0.023}$ & $ 1.063^{+0.002}_{-0.001}$ & $\rm 14.611^{+0.127}_{-1.253}$ & $ \rm 17.481^{+0.304}_{-0.303} $ & $ \rm 44.00/40 $ \\
$\rm 3$ & $\rm X-03-00$ & $\rm 53293.882$ & $ \rm 0.617^{+0.055}_{-0.021}$ & $\rm 0.059^{+0.005}_{-0.008} $ & $\rm 27.803^{+0.032}_{-0.032}$ & $ 1.055^{+0.001}_{-0.001}$ & $\rm 14.700^{+0.176}_{-0.438}$ & $ \rm 13.242^{+0.120}_{-0.120} $ & $ \rm 39.04/40 $ \\
$\rm 4$ & $\rm X-03-10$ & $\rm 53296.834$ & $ \rm 0.041^{+0.004}_{-0.004}$ & $\rm 0.128^{+0.004}_{-0.009} $ & $\rm 75.662^{+0.704}_{-0.699}$ & $ 2.804^{+0.010}_{-0.010}$ & $\rm 13.995^{+0.151}_{-0.149}$ & $ \rm 10.856^{+0.102}_{-0.102} $ & $ \rm 40.92/40 $ \\
$\rm 5$ & $\rm X-04-00$ & $\rm 53300.208$ & $ \rm 0.027^{+0.001}_{-0.0003}$ & $\rm 0.139^{+0.001}_{-0.002} $ & $\rm 84.784^{+1.265}_{-1.249}$ & $ 3.717^{+0.046}_{-0.046}$ & $\rm 10.476^{+0.091}_{-0.090}$ & $ \rm 13.355^{+0.156}_{-0.155} $ & $ \rm 41.69/40 $ \\
$\rm 6$ & $\rm X-04-10$ & $\rm 53302.689$ & $ \rm 0.026^{+0.0003}_{-0.005}$ & $\rm 0.140^{+0.055}_{-0.001} $ & $\rm 93.115^{+1.528}_{-1.506}$ & $ 3.660^{+0.158}_{-0.134}$ & $\rm 10.112^{+0.106}_{-0.105}$ & $ \rm 11.228^{+0.171}_{-0.171} $ & $ \rm 35.92/40 $ \\
$\rm 7$ & $\rm X-04-20$ & $\rm 53302.829$ & $ \rm 0.025^{+0.007}_{-0.003}$ & $\rm 0.140^{+0.004}_{-0.003} $ & $\rm 95.118^{+0.657}_{-0.654}$ & $ 3.745^{+0.022}_{-0.021}$ & $\rm 9.981^{+0.044}_{-0.044}$ & $ \rm 10.480^{+0.072}_{-0.071}$ & $ \rm 31.09/40 $ \\

$\rm 8$ & $\rm X-05-00$ & $\rm 53307.032$ & $ \rm 0.021^{+0.005}_{-0.003}$ & $\rm 0.120^{+0.001}_{-0.001} $ & $\rm 114.867^{+0.737}_{-0.733}$ & $ 3.519^{+0.024}_{-0.028}$ & $\rm 10.517^{+0.150}_{-0.140}$ & $ \rm 11.121^{+0.250}_{-0.249} $ & $ \rm 31.58/40 $ \\
$\rm 9$ & $\rm X-05-01$ & $\rm 53309.956$ & $ \rm 0.022^{+0.004}_{-0.004}$ & $\rm 0.111^{+0.017}_{-0.010} $ & $\rm 133.474^{+1.572}_{-1.556}$ & $ 3.505^{+0.032}_{-0.032}$ & $\rm 10.094^{+0.204}_{-0.200}$ & $ \rm 13.625^{+0.238}_{-0.238} $ & $ \rm 17.51/40 $ \\
$\rm 10$ & $\rm X-05-03$ & $\rm 53310.876$ & $ \rm 0.021^{+0.004}_{-0.003}$ & $\rm 0.115^{+0.015}_{-0.010} $ & $\rm 145.277^{+1.281}_{-1.273}$ & $ 3.309^{+0.023}_{-0.023}$ & $\rm 12.873^{+0.229}_{-0.224}$ & $ \rm 12.815^{+0.204}_{-0.203} $ & $ \rm 32.10/40 $ \\
$\rm 11$ & $\rm X-05-10$ & $\rm 53311.146$ & $ \rm 0.021^{+0.004}_{-0.001}$ & $\rm 0.127^{+0.006}_{-0.016} $ & $\rm 149.990^{+1.338}_{-1.329}$ & $ 3.267^{+0.021}_{-0.021}$ & $\rm 12.167^{+0.192}_{-0.189}$ & $ \rm 12.638^{+0.194}_{-0.194} $ & $ \rm 23.74/40 $ \\
$\rm 12$ & $\rm X-05-02$ & $\rm 53311.306$ & $ \rm 0.021^{+0.014}_{-0.004}$ & $\rm 0.126^{+0.002}_{-0.003} $ & $\rm 162.910^{+3.033}_{-2.980}$ & $ 3.041^{+0.053}_{-0.052}$ & $\rm 14.133^{+0.613}_{-0.641}$ & $ \rm 14.016^{+0.550}_{-0.549} $ & $ \rm 33.27/40 $ \\
$\rm 13$ & $\rm X-05-04$ & $\rm 53312.736$ & $ \rm 0.020^{+0.008}_{-0.002}$ & $\rm 0.128^{+0.010}_{-0.024} $ & $\rm 168.780^{+2.106}_{-2.078}$ & $ 3.237^{+0.033}_{-0.033}$ & $\rm 12.504^{+0.365}_{-0.354}$ & $ \rm 15.540^{+0.423}_{-0.422} $ & $ \rm 31.36/40 $ \\
$\rm 14$ & $\rm X-06-00$ & $\rm 53314.749$ & $ \rm 0.020^{+0.007}_{-0.002}$ & $\rm 0.127^{+0.007}_{-0.022} $ & $\rm 171.966^{+2.146}_{-1.900}$ & $ 3.135^{+0.025}_{-0.032}$ & $\rm 13.108^{+0.334}_{-0.325}$ & $ \rm 15.217^{+0.345}_{-0.344} $ & $ \rm 18.94/40 $ \\
\hline
\end{tabular}
\label{table:tcaf1}
\end{center}
\end{table}

\begin{table}
\tiny
\vskip0.2cm
{\centerline{\large Table \ref{table:tcaf2}}}
\caption{
TCAF Model Fitted Parameters in $2.5-25$ keV energy band for normalization, $N=N_{avg}=13.65$.
Here, we list the variations of disc accretion rate ($\dot{m_d}$) and halo accretion rate ($\dot{m_h}$) in Eddington units, shock location ($X_s$) in units of Schwarzschild radius, shock compression ratio ($R$) and mass of the BHC ($M_{BH}$) in $M_{\odot}$ with MJD, along with their errors.
The reduced ($\chi^2$) values for each case is also shown in the last column.
}

{\centerline{}}
\begin{center}
\begin{tabular}{c c c c c c c c c c}
\hline
\hline
$\rm Obs. $ & $ \rm Id. $ & $\rm MJD $ & $ \rm \dot{m}_d ~(\dot{M}_{Edd})$ & $ \dot{m}_h~(\dot{M}_{Edd}) $ & $ X_s~(r_S) $ & $ R $ & $ M_{BH}~(M_{\odot}) $ & $ N $ & $\chi^2/dof$ \\
\hline
$\rm 1$ & $\rm X-02-00$ & $\rm 53287.484$ & $ \rm 0.771^{+0.065}_{-0.022}$ & $\rm 0.068^{+0.008}_{-0.0003} $ & $\rm 29.153^{+0.027}_{-0.027}$ & $ 1.079^{0+0.001}_{-0.001}$ & $\rm 14.852^{+0.130}_{-0.128}$ & $ \rm 13.65 $ & $ \rm 36.81/41 $ \\
$\rm 2$ & $\rm X-02-01$ & $\rm 53290.036$ & $ \rm 0.730^{+0.020}_{-0.019}$ & $\rm 0.061^{+0.001}_{-0.002} $ & $\rm 28.808^{+0.025}_{-0.025}$ & $ 1.075^{+0.001}_{-0.001}$ & $\rm 14.491^{+0.165}_{-0.216}$ & $ \rm 13.65 $ & $ \rm 44.12/41 $ \\
$\rm 3$ & $\rm X-03-00$ & $\rm 53293.882$ & $ \rm 0.615^{+0.050}_{-0.012}$ & $\rm 0.059^{+0.003}_{-0.009} $ & $\rm 27.768^{+0.032}_{-0.032}$ & $ 1.054^{+0.001}_{-0.001}$ & $\rm 14.594^{+0.167}_{-0.125}$ & $ \rm 13.65 $ & $ \rm 38.71/41 $ \\
$\rm 4$ & $\rm X-03-10$ & $\rm 53296.834$ & $ \rm 0.039^{+0.004}_{-0.004}$ & $\rm 0.110^{+0.006}_{-0.004} $ & $\rm 79.041^{+0.494}_{-0.491}$ & $ 3.026^{+0.016}_{-0.016}$ & $\rm 12.772^{+0.127}_{-0.126}$ & $ \rm 13.65 $ & $ \rm 40.40/41 $ \\
$\rm 5$ & $\rm X-04-00$ & $\rm 53300.208$ & $ \rm 0.027^{+0.003}_{-0.003}$ & $\rm 0.139^{+0.016}_{-0.018} $ & $\rm 81.732^{+1.278}_{-1.260}$ & $ 3.700^{+0.046}_{-0.046}$ & $\rm 10.095^{+0.082}_{-0.081}$ & $ \rm 13.65 $ & $ \rm 41.68/41 $ \\
$\rm 6$ & $\rm X-04-10$ & $\rm 53302.689$ & $ \rm 0.024^{+0.002}_{-0.008}$ & $\rm 0.119^{+0.017}_{-0.015} $ & $\rm 93.727^{+1.872}_{-1.838}$ & $ 3.963^{+0.034}_{-0.033}$ & $\rm  9.356^{+0.061}_{-0.061}$ & $ \rm 13.65 $ & $ \rm 35.63/41 $ \\
$\rm 7$ & $\rm X-04-20$ & $\rm 53302.829$ & $ \rm 0.026^{+0.004}_{-0.001}$ & $\rm 0.130^{+0.009}_{-0.007} $ & $\rm 94.085^{+1.076}_{-1.068}$ & $ 3.883^{+0.086}_{-0.084}$ & $\rm 9.831^{+0.034}_{-0.034}$ & $ \rm 13.65$ & $ \rm 30.09/41 $ \\

$\rm 8$ & $\rm X-05-00$ & $\rm 53307.032$ & $ \rm 0.017^{+0.004}_{-0.001}$ & $\rm 0.128^{+0.018}_{-0.020} $ & $\rm 113.569^{+0.793}_{-0.788}$ & $ 3.538^{+0.014}_{-0.028}$ & $\rm 10.268^{+0.153}_{-0.151}$ & $ \rm 13.65 $ & $ \rm 31.19/41 $ \\
$\rm 9$ & $\rm X-05-01$ & $\rm 53309.956$ & $ \rm 0.022^{+0.004}_{-0.004}$ & $\rm 0.111^{+0.017}_{-0.010} $ & $\rm 133.302^{+1.573}_{-1.557}$ & $ 3.510^{+0.032}_{-0.032}$ & $\rm 10.082^{+0.204}_{-0.199}$ & $ \rm 13.65 $ & $ \rm 17.51/41 $ \\
$\rm 10$ & $\rm X-05-03$ & $\rm 53310.876$ & $ \rm 0.021^{+0.004}_{-0.003}$ & $\rm 0.114^{+0.013}_{-0.010} $ & $\rm 145.746^{+1.276}_{-1.270}$ & $ 3.321^{+0.023}_{-0.023}$ & $\rm 12.488^{+0.208}_{-0.205}$ & $ \rm 13.65 $ & $ \rm 32.10/41 $ \\
$\rm 11$ & $\rm X-05-10$ & $\rm 53311.146$ & $ \rm 0.020^{+0.004}_{-0.001}$ & $\rm 0.127^{+0.006}_{-0.016} $ & $\rm 150.742^{+1.335}_{-1.326}$ & $ 3.281^{+0.021}_{-0.021}$ & $\rm 11.700^{+0.177}_{-0.174}$ & $ \rm 13.65 $ & $ \rm 23.75/41 $ \\
$\rm 12$ & $\rm X-05-02$ & $\rm 53311.306$ & $ \rm 0.022^{+0.001}_{-0.001}$ & $\rm 0.125^{+0.002}_{-0.003} $ & $\rm 154.643^{+3.178}_{-3.117}$ & $ 2.957^{+0.050}_{-0.050}$ & $\rm 12.867^{+0.562}_{-0.538}$ & $ \rm 13.65 $ & $ \rm 33.28/41 $ \\
$\rm 13$ & $\rm X-05-04$ & $\rm 53312.736$ & $ \rm 0.020^{+0.008}_{-0.002}$ & $\rm 0.127^{+0.010}_{-0.024} $ & $\rm 166.567^{+2.131}_{-2.107}$ & $ 3.239^{+0.034}_{-0.033}$ & $\rm 13.282^{+0.408}_{-0.395}$ & $ \rm 13.65 $ & $ \rm 31.35/41 $ \\
$\rm 14$ & $\rm X-06-00$ & $\rm 53314.749$ & $ \rm 0.021^{+0.008}_{-0.002}$ & $\rm 0.126^{+0.008}_{-0.022} $ & $\rm 171.430^{+2.157}_{-1.788}$ & $ 3.135^{+0.025}_{-0.032}$ & $\rm 13.935^{+0.374}_{-0.364}$ & $ \rm 13.65 $ & $ \rm 18.94/41 $ \\
\hline
\end{tabular}

\label{table:tcaf2}
\end{center}
\end{table}

\begin{table}
\tiny
\vskip0.2cm
{\centerline{\large Table \ref{table:tcaf3}}}
{\centerline{Comparison of QPO frequencies obtained from theoretical predictions and actual fits when
$N$ is in the range $10-20$.}}
{\centerline{}}
\begin{center}
 \begin{tabular}{c c c c c c c c}

 Obs ID. & MJD & $M_{BH}~(M_{\odot})$ & $X_s~(r_S)$ & R & $\nu_{qpo}^{POS}$(Hz) & $\nu_{qpo}^{PDS}$(Hz) & $M_{BH}^{POS}~(M_{\odot})$ \\
 \hlin
 90115-01-03-10 & 53296.834 & 13.995$_{-0.149}^{+0.151}$ & 75.662$_{-0.699}^{+0.704}$  & 2.804$_{-0.010}^{+0.010}$ & 3.957$_{-0.112}^{+0.112}$ & 3.952$_{-0.166}^{+0.157}$ & 14.011$_{-0.547}^{+0.602}$ \\

 90115-01-04-00 & 53300.208 & 10.476$_{-0.090}^{+0.091}$ & 84.784$_{-1.249}^{+1.265}$ & 3.717$_{-0.046}^{+0.046}$ & 3.359$_{-0.145}^{+0.145}$ & 3.358$_{-0.144}^{+0.208}$ & 10.479$_{-0.620}^{+0.460}$\\
 \hline
\end{tabular}
\caption{The spectral parameters from TCAF fits $M_{BH}$, $X_s$ and $R$ are used in the formula obtained from POS for the determination of QPO frequency. The value is listed as $\nu_{qpo}^{POS}$ within errorbars. The mass $M_{BH}$ is then tuned further to reduce the difference between POS prediction and observed QPO $\nu_{qpo}^{PDS}$. The corresponding values is noted as $M_{BH}^{POS}$.}
\label{table:tcaf3}
\end{center}
\end {table}

\begin{table}
\tiny
\vskip0.2cm
{\centerline{\large Table \ref{table:tcaf4}}}
{\centerline{Comparison of QPO frequencies obtained from theoretical predictions and actual fits keeping
$N=N_{avg}=13.65$.}}
{\centerline{}}
\begin{center}
 \begin{tabular}{c c c c c c c c}

 Obs ID. & MJD & $M_{BH}~(M_{\odot})$ & $X_s~(r_S)$ & R & $\nu_{qpo}^{POS}$(Hz) & $\nu_{qpo}^{PDS}$(Hz) & $M_{BH}^{POS}~(M_{\odot})$ \\
 \hlin
 90115-01-03-10 & 53296.834 & 12.772$_{-0.126}^{+0.127}$ & 79.041$_{-0.491}^{+0.494}$  & 3.026$_{-0.016}^{+0.016}$ & 3.758$_{-0.092}^{+0.092}$ & 3.952$_{-0.166}^{+0.157}$ & 12.156$_{-0.475}^{+0.521}$ \\

 90115-01-04-00 & 53300.208 & 10.095$_{-0.081}^{+0.082}$ & 81.732$_{-1.260}^{+1.278}$ & 3.700$_{-0.046}^{+0.046}$ & 3.697$_{-0.162}^{+0.162}$ & 3.358$_{-0.144}^{+0.208}$ & 11.125$_{-0.656}^{+0.487}$ \\
 \hline
\end{tabular}
\caption{Spectral parameters from TCAF fits $M_{BH}$, $X_s$ and $R$ are used in POS model for the determination of QPO frequency. The value is listed as $\nu_{qpo}^{POS}$ within errors bars. The mass $M_{BH}$ is then tuned further to reduce differences between POS prediction
and observed QPO $\nu_{qpo}^{PDS}$. The corresponding value is noted as $M_{BH}^{POS}$.}
\label{table:tcaf4}
\end{center}
\end {table}

\section{Discussions and Conclusions}

In this paper, we investigate evolution of spectral properties of the Galactic
BHC H1743-322 during the declining phase of the 2004
outburst to study the accretion flow dynamics and to extract the mass of the
BH independently from each observation. This was the first `normal' outburst after about 20 years. However,
data during hard and hard-intermediate states in the rising phase is missing and
since then it was mostly in soft states except towards the end of the declining phase.
Hence we concentrate our study only in this end phase
as we expect interplay between the two flow components of TCAF models.
We successfully addressed the evolution of accretion rates of both disc and halo, shock location
(which represents the size of the Compton cloud) and the compression ratio to have a clear understanding of the outburst.
It is important to note here that the fits obtained by spectral models, such as \textit{diskbb + power law}, does not provide
any clue about the mass of the object, neither does it explain the accretion flow dynamics around the BHC.
TCAF solution, on the other hand, gives an independent estimate of $M_{BH}$ from every single observation.

Molla et al. (M16a) obtained the mass of the black hole in the range $11.2^{+1.66}_{-1.95} M_{\odot}$.
Further, they estimated the mass of the BH with other methods such as
Shaposhnikov \& Titarchuk 2007 (ST07) using the  Photon Index-QPO frequency correlation technique. The measured mass of the black hole was obtained as $11.61\pm0.62M_{\odot}$. Shaposhnikov \& Titarchuk (2009, ST09) predicted the mass of the black hole to be $13.3\pm3.2M_{\odot}$ using the correlation between their spectral and timing properties while McClintock et al. (2009), estimated the mass $\sim 11.0 M_{\odot}$ using their high frequency QPO correlation method. From the model of high
frequency QPOs based on the spin of the black hole P\'{e}tri (2008) obtained the mass of the BHC in the range of $9-13 M_{\odot}$.
We have obtained the mass of the black hole in the range  $10.31 M_\odot - 14.07 M_\odot$ which agrees well with these
previous measurements.

The PCA spectra of the object clearly show that most of the flux is contributed from the soft photons emitted by the disc.
The flux emitted from the disc is $\sim T^4$ and draws its energy from the loss in gravitational potential energy $\sim \frac{GM_{BH}}{r}$.
Thus, roughly the spectra obtained by the best fit with TCAF has an intrinsic dependence of $T$
on $M_{BH}$ as $M_{BH}\sim T^4$. The spectra at low energy, where the blackbody radiation from the disc is dominating,
is limited by the resolution of RXTE/PCA. Any error in the measurement, combined with the error in
the fit parameters which depend on $T$, leads to a significant proportional error
in the determination of $M_{BH}$. Despite that, the mass is found to lie in a narrow range
which conforms and restricts further, the previous findings by M16a and P\'{e}tri et al. (2008).

We assumed that the mass, distance and inclination angle of the object are constant such that
the projected area of the disc along the line of sight does not change keeping the model normalization
more or less unchanged provided the instrument response function and the absorption from
intervening medium are determined correctly which may affect Normalization also. Furthermore, we assumed that
there was no contribution to X-rays from the jet.
However, since mass, distance or inclination angle are not accurately known and the
RXTE resolution is low to generate accurate spectra, we allowed to
vary both mass and normalization within a narrow range. We also used the average normalization and repeated our analysis.
We found reasonably good $\chi^2$ values as evident from table \ref{table:tcaf1} and table \ref{table:tcaf2}. The average reduced $chi^2$ value is $\langle \chi^2_{red} \rangle = 0.82 \pm 0.20$ for $10<N<20$ and $\langle \chi^2_{red} \rangle = 0.79 \pm 0.19$ for $N=N_{avg}=13.65$. We believe that unless the system parameters (most importantly inclination angle for a precessing disc) change, this Normalization may be used to analyze
subsequent outbursts.

The low-frequency of QPO derived from the power density spectrum fitted parameters was found
to be in agreement with the one obtained from the POS model if the systematic error is considered.
The velocity of the shock front $v_s$ using the POS model was found to be similar to those
with the previous work by Debnath et al. (2013).

The masses obtained by the POS model for both the cases with free and constant normalization agree with the range ($10.31~M_{\odot}-14.07~M_{\odot}$) obtained by the spectral fits with a constant, averaged normalization of $N=N_{avg}=13.65$. The POS model provides a secondary verification to our method and reflects upon the general consistency of our approach. We thus conclude from our analysis that the mass of the BHC is in the range $10.31~M_{\odot}-14.07~M_{\odot}$.

TCAF solves the radiative transfer equation for a steady state two component flow to discuss about the
spectral properties. The day-to-day evolution of the spectra are, thus, explained in terms of the
variation of physical parameters which are used in TCAF. This allows us to have a fresh estimate of the
mass of the black hole, independent of any other observations. The POS model predicts values of QPO frequencies from the spectral
parameters, and we find that observed QPOs are of similar values. Thus TCAF self-consistently
puts spectral and timing properties under a common framework. The derived mass is well
within the range estimated by earlier workers using very different observational data, and model. Presently,
TCAF does not incorporate effects of magnetic fields, spin of the black
hole or line emissions. These effects are being incorporated and results would be reported elsewhere.

redpajama_set_name: RedPajamaArXiv


Interesting. It'll be interesting to see what they do to Warudaros.
Well that's the way to do it. If you're worried about the bad guys not selling well, only make one figure but make it a combining troop builder.


HAMPTON — Doris D. Marsolais, 79, died Monday, July 27, 2009, at Country Rehabilitation & Nursing Center in Newburyport, Mass.
She was born Aug. 3, 1929, in Amesbury, Mass., the daughter of the late Hormidas and Evelyn (Broulliard) St. Germain.
She was a 1947 graduate of Amesbury High School.
Mrs. Marsolais was employed in the dining hall at Governors Academy in Byfield, Mass., for 15 years.
The widow of Robert P. Marsolais, her husband of 56 years who died March 10, 2008, she is survived by one son and his wife, Gary P. and Debra Marsolais of Kensington; one daughter and her husband, Lee Ann and David Kelley of Hampton; two grandchildren, Colin P. Kelley and Robert L. Kelley, both of Hampton; three brothers and their wives, Roger and Persis St. Germain of West Andover, Mass., Joseph and Shirley St. Germain of Groveland, Mass., and Maurice and Terry St. Germain of Methuen, Mass.; one sister, Pauline Macey of Salisbury, Mass.; and several nieces and nephews.
WE REMEMBER: She made her home in Newburyport for most of her life before moving to Hampton in 1986, where she and her late husband experienced many years of enjoyment by the ocean they loved so much.
She was a communicant of St. Theresa Church, Rye Beach.
The special friendships she enjoyed over the years at Governors Academy were honored by the students and faculty just prior to her retirement in 1989 with the dedication of the school yearbook to their beloved "Doris."
She was a loving mother and friend to her two children and their spouses. Aside from her immediate family and friends, she found her greatest source of enjoyment, comfort and pride in her two grandsons.
The family would like to express their gratitude to the nurses and staff at the Country Rehabilitation & Nursing Center in Newburyport for their exceptional and loving care. Their tremendous support, help and friendships are of great comfort. They also thank the nurses and volunteers of North Shore Hospice, Danvers, Mass., for their professionalism and dedication.
A Mass of Christian burial will be celebrated Saturday, Aug. 1, at 10 a.m. in St. Theresa Church, 815 Central Road, Rye Beach, with a reception immediately following in the Parish Center.
Memorial donations may be made to the American Cancer Society, 30 Speen Street, Framingham, MA 01701, or to St. Jude Children's Research Hospital, 501 St. Jude Place, Memphis, TN 38105.


"It is a great pleasure to announce that Hugo Doyon-Karout is now part of Beyond Creation as our new bass player!
"Being a very talented, forward thinking musician and a 6 string fretless bass player as well, he proved himself to be right what we needed to complete our formation. As most of you may not know, Kevin and Hugo have been playing together with our brothers in Brought By Pain for the past 3 years, allowing us to develop a close friendship and musical synergy along the way. It is the start of an exciting and inspiring experience for us and we'd like to thank every fan for their supportive attitude towards our evolving musical journey."


How Much Water do Fennec Foxes Need? How Long to Dehydrate?
Fennec Foxes can tolerate long durations without water.
Out of the fourteen carnivorous species of animals living in the Sahara, this species is the only one that can live away from water. For the most part, the little Fennec relies on berries and grass for its water intake.
Physiologically, their kidneys are also adapted to restrict water loss. Being nocturnal and living deep underground helps prevent water loss as well. Burrowing may also cause the formation of dew, which may be consumed by the little Fox.
However, it does not mean that it will refuse water if it sees any. The Fox will still consume water, if it is available.
Desert plants are also a good source of water for the Fennec, just as it may be water source for many other desert animals too. These Foxes can live for years without drinking water by relying heavily on the desert plants alone.
What about the babies? The baby Fennec drinks its mother's milk for only about a month before moving on to solid foods, very much unlike most other mammals. This directly correlates to its gestational period of only 52 days.
The super large ears of this Fox also helps dissipate heat to keep it cool during the day. That way, the little fox need not worry about needing too much water to stay cool. Its coat also helps keep it warm during the night when the weather is cold but dry.
Does a Fennec take any shower? Very little research has been done about this little fox, but when it comes to shower, domesticated Fennecs owners will have no worries about giving it a good time. But of course, just like any other pets, do not let the little Fox bath for too long, otherwise it might catch a cold (and that will mean an expensive bill from the vet!).


I don't think many hen nights turn into a knitting retreat, but it's the logical solution when every participant is a knitter. One of my best friends is getting married later this year and we all met up in Yorkshire for a weekend of knitting and relaxation. I had been to Yorkshire before for work, but I had never had a chance to spend time in a stunning landscape filled with textile heritage.
We took the train from Carlisle to Settle - to our great surprise (and delight) the train journey turned out to be spectacular. It runs past the Pennines and through the Yorkshire Dales.
Every station was a Victorian delight with ornate architecture and beautiful details. I can only recommend taking the train journey - it is absolutely stunning and I feel fortunate to have experienced it.
And there are sheep everywhere. I was particularly interested in seeing the varieties of sheep in the fields we passed. The Swaledale sheep is the official 'face' of the Yorkshire dales and I spotted a few on my train journey. I am not Deb Robson, so I could not identify all the little dots scampering around the fells but it was still great seeing so many varieties.
We had rented a house a few miles outside Settle. It was pretty much my dream house: Georgian proportions, a country kitchen (though I found cooking on an AGA fairly intimidating), a small conservatory with built-in book shelves and open fires in each of the living rooms. Did I mention the views?
This was the view from my bedroom (where I sat in the window seat as I took this picture). It looked like merino sheep in the cow-parsley/buttercup field. They fled as soon as I tried getting closer for a better view. Roses in the front garden and a beautiful back garden with views across the dale.
It was a bit too cold for me to sit outside and knit, but I was tempted! Once inside, the house offered many temptations..
.. but I stuck to my knitting mostly. I currently have three projects on the go - one that requires a lot of maths, one that requires a lot of concentration and, er, one that's 1 ply lace. I mainly worked on the latter as it seemed more straightforward given the high level of hilarity.
I did not move from my comfy chair most of the weekend, though I discovered just how bad I am at playing pool. The adjacent house had a ruby spaniel that loved cuddles, so time was spent doing that too. And copious amounts of tea, tea and tea. Cake was had from the interestingly-named local pub/bakery.
It was a lovely weekend. We took the train back to Carlisle yesterday.
And then a rail-replacement bus back to Glasgow (when I fell asleep - all that fresh country air!). I'm having the day off today as I'm oddly exhausted after my relaxing weekend away. While it was fun waltzing around a 19th country house for a few days, it's rather lovely to be home in my humble abode again. I'm down to London next week - when I pass Carlisle on my way down, I'll think fondly of this trip.
I'm supposed to be enjoying a long bank holiday weekend, so this blog post will be short and sweet. All photos by Mr D. who has lately begun taking more abstract photos and I'm enjoying looking at the world through his eyes.
First, thank you to everybody who made the trek to the Fluph yarn shop in Dundee this past Saturday for Yarn Shop Day. I lost track of quite how many people dropped by but I loved saying hello to all (including the dogs that people so thoughtfully brought along). I also loved seeing all the knitwear on display - from a stunning Aidez cardigan to the most exquisite cobweb Shetland "wedding ring" shawl.
Later this month I am heading to Yorkshire for another knitting retreat (I'm combining it with seeing far-flung friends). However, I've had yet another jury citation - this is the third since November - so my retreat plans may be cut short. I love spending time in Yorkshire, I very rarely get to see these friends and the retreat location includes a short stroll to a delightful yarn shop, so fingers crossed everything works out. I know many of you wonder about knitting retreats - while you obviously have the option of arranging one for yourself, there are a few lovely 'open' retreats. Helen Lockhart of Ripples Crafts has been running a regular knitting retreat on Tanera Mor, an beautiful island off the Scottish North-West coast, and I know she is planning more retreats in the Scottish Highlands. You could also opt to spend time in the beautiful Welsh countryside together with Brenda Dayne (of Cast On podcast fame) and Felicity Ford at the Gwlana retreat. I am sure there are other retreats scattered around the British isles - do share your info in the comments section if you know of any!
Finally, thank you for all your kind words about the passing of my art teacher. It was a hard post to write.
I am really enjoying all the Byatts popping up both on Ravelry and at the events I attend. While my own group's KAL officially ended at the end of March, several other KALs have strung up. It's such a marvellous thing to see all the colour combinations and personal touches out there. As I enjoy looking through all the project photos, I thought I'd share a couple of the finished Byatts with you. First up is JessieMcKitrick who chose to combine a rich red-purple with a stunning gold colour. This warm colour combination is rich and sumptuous - and it reminds me quite a bit of the Game of Thrones series wherein crimson and gold are the colours of the royal house of Lannister. Hey, I happen to live with someone who has read all the books..
Continuing on with the gold theme, I gasped when I first saw the colour combination that CountrySinger had chosen for her version. I have mild synaesthesia and those two colours vibrate when I look at the photos. I especially love how it's miles outside my own comfortzone and yet I'd wear it in a heartbeat. Now that is colour appreciation for you!
Whitehart, aka Sadie, chose to stash-dive for her Byatt. I chose this photo because I think the blue-turquoise looks so stunning on Sadie and works incredibly well with her skin tone. I know many people have been focused on getting the contrast colour right, but here Sadie shows why it's even more important to get the main colour right. This colour combination suits her so well.
I have seen the next Byatt in person and it looks so delicate. EllaSkye ran into the problem of not having enough yardage to complete the pattern as written. Her solution was to add a third colour that was a slightly darker shade of her original main colour and she opted to do the cast-off in the darker colour too so the shawl had a strong sense of continuity. It looks amazing and even prettier when you get to see it and squish it in person, I can tell you that.
Another Byatt I have seen in person: Helen of RipplesCraft. Helen chose a very contemporary colour combination of a neutral slate gray (she calls it 'peat' - who am I to debate colour with a dyer?!) and a zingy lime green. I love how this makes the stripe section sing.
Finally, Noirem's Byatt. I will confess that this photo stopped me in the tracks. A beautiful combination of subtle blue-teal with a silvery contrast colour and then the stunning shawl pin that echoes the cast-off edge. I knitted my original Byatt in a warm teal with a bronze-like edging. Jennifer has somehow made a cool, elegant twin version of that shawl.
A lot of other Byatts out there - I've seen gradient versions, glittery versions, and variegated versions. I have somehow managed to design a shawl that lends itself to a lot of experimentation with yarns and I'm really proud of that. Keep uploading those photos. I adore seeing every single one.
PS. I cannot resist linking to this thoughtful post about knitting Byatt. It really stopped me in my tracks.
To my great delight and surprise, my partner whisked me away on a trip to the Isle of Arran this weekend. The Isle of Arran is about two hours away from Glasgow by train and ferry, but I had never been.
I twigged I had arrived among kindred spirits when we noticed small sheep statues along the coast.
The easiest way to get around Arran is by bus - we asked to get dropped off at Sannox about 8 miles north of the ferry terminal. Sannox stems from the Viking place name "Sand Vik" (Sandy Bay) - always a pleasure to see places my Viking ancestors have been!
We headed towards Glen Sannox - the walkers' guide labelled this "an easy ramble with stunning scenery". The first part of the path was easy (and we stopped to eat brambles - Arran clearly has a micro-climate quite unlike the mainland).
The path into Glen Sannox became less friendly (and more boggy) after we crossed the stream. We walked towards Coire na Ciche (The Devil's Punchbowl) with the slopes of Goatfell on our left and the peaks of Cir Mhor and Caisteal Abhail in front of us. I was worried about how my injured left knee would hold up (especially as the path was not as gentle as we had imagined) - but although I was in pain, I did not have to resort to the heavy-duty pain killers and my knee only caused me to stumble occasionally.
We couldn't resist a selfie (though I look odd!). I wore my trusty Snorri jumper and i have a bit of a story to tell about the hat I'm wearing - but that's for another day.
No filter! When the sun came out, the colours were breathtaking. The clouds rolling over Cir Mhor (the peak in perpetual cloud) kept getting darker, though, and the already brisky wind got stronger. It was a beautiful, rich landscape. Wildlife was all around us too - we saw so many red deer that we got jaded (though I am sure they were not "wild" animals, just "managed"), various birds, the ever-present sheep and I even caught the eye of a little adder. But it was clear that we needed to head back before the clouds caught up with us.
It was just after midday, but it felt later. We retraced our steps, had the last of our packed lunch and then caught the bus (the bus - there are no other busses on Arran) making an almost full-circle of the island before going home.
What a lovely, special day. I don't get to go on adventure with my partner as much as I'd like but our trip to Arran was just perfect: stunning scenery, the best company in the world, apples in the backpack and I even cast on something very special whilst there. Magic.


According to data released by Tokyo Shoko Research on September 8, one in ten residents in Tokyo's Minato ward are company presidents, making it the most highly concentrated of all of Tokyo's 23 wards. Minato was closely followed by Chiyoda and Shibuya wards which both have a concentration of 8.62%.
Katsushika ward had the lowest percentage with 2.40%.
In terms of total residents, Setagaya was in top place with 38,771 company presidents, accounting for 4.31% of the ward's population and 10.91% of the population of the 23 wards. Although Setagaya is mostly a suburban area located some distance from the main business districts, the population surged during Japan's rapid economic growth years in the 1970s. In the past, the development of high-end residential neighbourhoods, including Seijo and Jiyugaoka, were popular with wealthy Japanese looking for large homes and leafy streets. In recent years, however, there have been signs of a shift of wealthy residents from outer suburbs like Seijo and Denenchofu to more conveniently located and spacious apartments in central Tokyo.
In terms of industry, 15.1% of the company presidents residing in Shibuya ward were involved in telecommunications/information industries. In the late 1990s, Shibuya ward became Japan's IT headquarters, with a number of IT-related venture businesses and start-ups centering their operations around the Shibuya Station area. The area became known as Bit Valley. This hub is looking at being revived in the coming years as the station area is redeveloped.
Source: Tokyo Shoko Research, September 8, 2017.
Предлагаем вам со скидкой https://ford.niko.ua у нашего менеджера.


I have to say, being away from home makes you appreciate the little things. It also makes you crazy. The hour-long lines for breakfast, lunch and dinner; the immensely crowded hallways, the endless rain… it's all stuff I could live without.
Friday, I went to a class that, I thought, was going to be about team bonding. It ended up being about how to get good quotes. I guess it pays to read the class descriptions.
I didn't feel so well at night, so I had to skip out on the dance. However — there are definitely positives about this trip.
All in all, it has been a good trip. I'm looking forward to being home tomorrow, but not so much going back to school. There's a bit of nostalgia, too, this being my last convention. :[ Better make tonight the best!


T.C. Prosser 1854 map shows the location of the chapel on the south-east corner of King Street at Chapel.
The red brick church was sold to the Village of Bolton as their Town Hall.
Primitive Methodist brick church built in 1873.


text:
IPL 2018 >
IPL 2018, RR vs CSK: Rajasthan Royals, Chennai Super Kings look to regain lost momentum
Updated Apr 19, 2018 | 13:53 IST | PTI
With two wins and two defeats, Rajasthan Royals are fifth with four points, while Chennai have also gathered an equal number of points with two victories from three matches. A loss in their last outing has hurt both the former champions and they will look to get back to winning ways when they face off.
File image of Chennai Super Kings' Dhoni in action against Rajasthan Royals | &nbspPhoto Credit:&nbspBCCL
Rajasthan Royals and Chennai Super Kings, the two franchises that returned to the IPL after serving bans in the aftermath of the 2013 spot-fixing scandal, will come face to face for the first time in the ongoing edition, keen to regain lost momentum. A loss in their last outing has hurt both the former champions and they will look to get back to winning ways when they face off. With two wins and two defeats, Rajasthan Royals are fifth with four points, while Chennai have also gathered an equal number of points with two victories from three matches. They are placed fourth because of better net run rate.
Both the teams were missing in action owing to a two-year ban for corruption. Rajasthan, under new captain Ajinkya Rahane, had a bad start to the campaign but they have done well with two back-to-back wins before Kolkata Knight Riders outclassed them by seven wickets. On a slow wicket, Rahane and Co. failed to stitch partnerships and ended up with a below-par total of 160-8 on board, which KKR chased down with consummate ease, losing three wickets.
Sanju Samson has been the batting star for Rajasthan as he has scored 185 runs so far with an unbeaten 92-run innings being the highlight but he didn't get the desired support from other batsmen.
Rahane has made some useful contributions but he failed to capitalise on the starts.
Their bowling unit, led by K Gowtham and Ben Laughlin, have done well. They sustained the onslaught by big hitters like Virat Kohli and A B de Villiers during their match against heavy-weight Royal Challengers Bangalore.
But England all-rounder Ben Stokes, who was bought for a whopping Rs 12.5 crore by Rajasthan, has been a big let down and he needs to live up to the billing.
Two-time champions Chennai, on the other hand, made a rampaging start to their campaign with back-to-back wins against defending champions Mumbai Indians and Kolkata Knight Riders.
While Dwayne Bravo came to their rescue with a 30-ball 68 against Mumbai Indians in their first match, it was Sam Billings who put the finishing touch to their superb runchase against Kolkata Knight Riders in a high-scoring match.
In their last match against Kings XI Punjab, Ambati Rayudu (49) and MS Dhoni (79) brought the Super Kings close to the victory target of 198 before falling short by four runs.
Among bowlers, Shane Watson and Shardul Thakur led the pace attack for Chennai with five and three wickets respectively, while Imran Tahir did the job with his Leg-break googlies.
The experienced spin duo of Harbhajan Singh and Ravindra Jadeja too can be a potent force.
Teams (From):
Rajasthan Royals: Heinrich Klassen, Benjamin Stokes, Jaydev Unadkat, Sanju Samson, Jofra Archer, Krishnappa Gowtham, Jos Buttler, Ajinkya Rahane, Darcy Short, Rahul Tripathi, Dhawal Kulkarni, Zahir Khan Pakteen, Ben Laughlin, Stuart Binny, Dushmantha Chameera, Anureet Singh, Aryaman Vikram Birla, Midhun S, Shreyas Gopal, Prashant Chopra, Jatin Saxena, Ankit Sharma, Mahipal Lomror.
Chennai Super Kings: MS Dhoni (capt), Suresh Raina, Ravindra Jadeja, Faf du Plessis, Harbhajan Singh, Dwayne Bravo, Shane Watson, Kedar Jadhav, Ambati Rayudu, Deepak Chahar, KM Asif, Kanishk Seth, Lungi Ngidi, Dhruv Shorey, Murali Vijay, Sam Billings, Mark Wood, Kshitiz Sharma, Monu Kumar, Chaitanya Bishnoi, Imran Tahir, Karn Sharma, Shardul Thakur, N Jagadeesan.
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redpajama_set_name: RedPajamaCommonCrawl


There has been much research on the effects of banking crises, but corporate resilience to systemic crises is less well understood. This column uses data from 34 countries from 1990 to 2011 to analyse the role of social trust – societal expectations that people will behave honestly and cooperatively – in building corporate resilience. It finds that social trust facilitates access to trade credit, and dampens the harmful effects of crises on corporate profits and employment.
Most commentators agree that a European banking union would end the 'deadly embrace' between creditors and governments. This column argues that a banking union would be welcome, but that current proposals are dogged with problems. To resolve these, we should stop discussing debt restructuring and instead enhance the borrowing capacity of the European Stability Mechanism. A programme to buy capital in financial institutions unable to raise it directly on the market should also be set up.
A combination of shocks has led to the spectre of a renewed systemic bank crisis within the EU. This column argues that what is needed is a regulatory policy response in the form of joint action by European governments to convince financial investors that bank liabilities are secure.
Cyprus has been striving to get back on its feet after a painful bailout in 2013. This column examines the lessons that could have been drawn from the Cypriot experience by Greece in its recent attempt to seal a bailout deal. Specifically, lengthy negotiations – while tending to mitigate the risk of contagion – offer little benefit for debtor countries, and capital controls, once implemented, cannot be easily undone. While they come too late for Greece, these lessons can be important for countries in need of financial assistance in the future.
This paper argues that the European banking crisis can in part be explained by a "carry trade" behavior of banks. The results are supportive of moral hazard in the form of risk-taking by under-capitalized banks to exploit low risk weights and central-bank funding of risky government bond positions.
The recent IMF assessment of Europe's financial sector found that much has been achieved to address the recent financial crisis in Europe, but vulnerabilities remain, and intensified efforts are needed across a wide front, one of which being bank balance sheet repair. This column looks at progress with bank restructuring in Europe.
The euro cannot have a centralised monetary authority and decentralised bank supervision. This column draws on US banking history, detailing how a banking crisis in the nineteenth century led to the creation of dual systems of bank supervision. The US system was imperfect, and the central role and powers of the ECB within the Single Supervisory Mechanism will be to limit the weaknesses of a dual system of supervision. Despite this, hazards remain. For those looking for a guide to the potential threats to financial stability under this system, understanding the US experience is relevant.
Broadly speaking, there are three types of economic crisis: banking crises and panics, credit frictions and market freezes, and currency crises. This column argues that features from these types of crises have been at work and interacted with each other to shape the events of the last few years. From an extensive review of literature on these issues, it's clear that the biggest challenge policymakers and economists face is in developing integrative models that better describing contemporary economic realities.
This paper adds the Bernanke-Gertler-Gilchrist model to a modified version of the Smets-Wouters model of the US in order to explore the causes of the banking crisis. The authors find that banking crises occur on average once every 40 years and around half are accompanied by financial crisis. Financial shocks on their own, even when extreme, do not cause crises, provided the government acts swiftly to counteract such a shock.
Much of macroeconomic policymaking is trial and error. This column discusses calamitous error on the part of Iceland's policymakers, in the hope that others can at least try something else.
Is Iceland perhaps too small to be sustainable as a sovereign state? This column argues there are many reason why small is beautiful. Even though they do not benefit from scale economies and large pools of talent, small countries with cohesive societies can be successful as long as they are open to the world. Still, Iceland stands to gain from joining the EU.
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text:
Риалут Серж Вохор (, 1955) — премьер-министр Вануату.

Биография

Ранние годы
Серж Вохор родился в 1955 году на крупнейшем острове Вануату, Эспириту-Санто, в городе Порт-Олри. Школьное образование получил в Школе Святой Анны (), затем обучался в одном из лицеев Порт-Олри, а в 1974 году практиковался в качестве медицинского работника.

Политическая карьера
Серж Вохор является членом Союза умеренных партий, консервативной, франкоязычной политической партии Вануату. Когда его партия пришла к власти в 1991 году, Вохор стал министром иностранных дел Республики, оставаясь им до 1993 года, а в декабре 1995 года впервые в своей политической карьере — премьер-министром Вануату, находясь на посту до февраля 1996 года. Повторно Вохор становился премьер-министром страны в сентябре 1996—марте 1998 годов, июле—декабре 2004 года.

После того, как на парламентских выборах 1998 года Союзу умеренных партий не удалось образовать коалиционное правительство, Вохору удалось остаться членом правительства, выступая с 1999 по 2001 года в качестве министра иностранных дел Вануату. После парламентских выборов 2002 года он также занимал пост министра иностранных дел с 2002 по 2003 года, а также был заместителем премьер-министра. В 2002 году, в интервью газете The Melbourne Age Вохор, обвинил австралийскую федеральную полицию в шпионаже через прослушивание телефонов на территории Вануату и в попытке дестабилизации политической системы страны. В 2003 году в качестве министра иностранных дел он также выступил с критикой американского правительства и его союзников, которые начали военную операцию на территории Ирака.

Несмотря на потерю Союзом умеренных партий нескольких мест в парламенте по результатам выборов 2004 года, Вохору удалось сформировать коалицию с независимыми парламентариями и членами других партий, что позволило ему вновь быть избранным в качестве премьер-министра Вануату. В ходе голосования он получил поддержку 28 депутатов, в то время как его главный оппонент, Хам Лини, получил 24 голоса. В следующем месяце Вохор сформировал правительство национального единства, в котором Лини стал заместителем премьер-министра.

В ходе третьего премьерского срока Вохора произошло несколько противоречивых событий. Так, в сентябре 2004 года новый премьер-министр подверг резкой критике любые попытки иностранных государств вмешиваться во внутреннюю политику Вануату, в том числе, была затронута проблема австралийских военных консультантов на территории страны, часть из которых занимала определённые должности в полиции и мобильных силах Вануату. В результате, министр иностранных дел тихоокеанской республики Барак Сопе потребовал вывода с территории страны представителей австралийской федеральной полиции, глава которой, в свою очередь, выразил опасения, что этот шаг может привести к появлению в Вануату международных наркотических синдикатов и созданию лабораторий по производству амфетаминов.

Одним из самых противоречивых событий третьего премьерского срока Вохора стал визит 3 ноября 2004 года в столицу Тайваня, город Тайбэй, в ходе которого он установил дипломатические отношения с Республикой Китай (Тайвань) без одобрения Совета министров Вануату (первый коммюнике о взаимном признании был подписан ещё в 1992 году). Сделано это было спустя два месяца после визита в КНР, во время которого лидеры двух стран договорились о выделении Вануату помощи в размере $10 млн. Кроме того, КНР уже оказывал этой меланезийской стране помощь, в том числе, выделил средства на строительство здания Парламента Вануату, корпуса Южнотихоокеанского университета, Колледжа сельского хозяйства и Министерства иностранных дел. После установления дипломатических отношений с Тайванем КНР пригрозил приостановить финансовую помощь Вануату. Через некоторое время так же поступила и Австралия, которая обвинила правительство Вануату в коррупции и беззаконии, чем вызвала недовольство правительства Тайваня. В Совете министров Вануату, в свою очередь, было проведено голосование, результатом которого стало аннулирование договорённостей с Тайванем и признание только одного Китая, Китайской Народной Республики. В течение нескольких недель и РК, и КНР на фоне продолжавшихся разногласий в правительстве Вануату имели свои дипломатические миссии в Порт-Вила. Лишившись поддержки 16 членов парламента и, таким образом, потеряв большинство, Вохор мог потерять свой премьерский пост ввиду того, что оппозиция попыталась вынести ему вотум недоверия. В ответ Вохор обратился в Верховный суд Вануату, утверждая, что, исходя из новых конституционных поправок, премьер-министр не может быть смещён со своей должности в течение первого года исполнения своих обязанностей. Тем не менее Верховный суд вынес решение, согласно которому эти поправки ещё не были одобрены на всенародном референдуме, а значит, не вступили в законную силу. 11 декабря 2004 года Вохор был смещён Хамом Лини. С тех пор до апреля 2011 года он оставался лидером оппозиции в парламенте Вануату.

24 апреля 2011 года вновь возглавил правительство, после того как парламент вынес вотум недоверия премьер-министру Сато Килману. Однако уже 13 мая Вохор покинул свой пост, так как Верховный суд признал его избрание неконституционным. Он получил ровно половину голосов депутатов — 26 из 52.

Примечания

Премьер-министры Вануату
Википедия:Персоналии, не категоризованные по месту рождения
Министры иностранных дел Вануату

redpajama_set_name: RedPajamaWikipedia


Naturally though, the kids are excited and can't wait to celebrate, and there's some great ways you can get into the spirit of the season outdoors with your students.
Have a Christmas picnic – ask your students to bring in some goodies to share (make sure you set some limits so you don't end up with 20 trifles or 30 Christmas puddings!) and head outside for a bite to eat. Bring some tinsel to make it festive, but don't forget to clean up afterwards.
Is your class filled with arty types? Why not make some natural Christmas decorations!