text:
Q: I useing asp.netcore3.1 and I want read post request params from webservice but missing request params when using https? I create a filter to authentication http request like below:

    public class UseSSLAttribute : AuthorizationFilterAttribute
    {
        public override void OnAuthorization(System.Web.Http.Controllers.HttpActionContext actionContext)
        {
            if (actionContext.Request.RequestUri.Scheme != Uri.UriSchemeHttps)
            {
                HttpResponseMessage msg = new HttpResponseMessage();
                msg.StatusCode = HttpStatusCode.Forbidden;
                msg.ReasonPhrase = "SSL Needed!";
                actionContext.Response = msg;
            }
            else
            {
                base.OnAuthorization(actionContext);
            }
        }
    }

and then use this filter for below action that call by webservice and read parameters from request. but when using https missing parameters but in http every parameter has value.
 [UseSSL]
       [RequireHttpsAttribute]
        public ActionResult SuccessPayment()
        {

            ViewBag.Bank = "ملت";
            string SaleReferenceId = "0";
            string ResCode ="0";
            string SaleOrderId = "0";
            string RefId = "0";
            var gg = "";
            if (Request.HasFormContentType == true)
            {
                if (Request.Form.ContainsKey("SaleReferenceId") == true)
                    SaleReferenceId = string.IsNullOrEmpty(Request.Form["SaleReferenceId"]) ? "0" : Request.Form["SaleReferenceId"].ToString();
                if (Request.Form.ContainsKey("ResCode") == true)
                    ResCode = string.IsNullOrEmpty(Request.Form["ResCode"]) ? "0" : Request.Form["ResCode"].ToString();
                if (Request.Form.ContainsKey("SaleOrderId") == true)
                    SaleOrderId = string.IsNullOrEmpty(Request.Form["SaleOrderId"]) ? "0" : Request.Form["SaleOrderId"].ToString();
                if (Request.Form.ContainsKey("RefId") == true)
                    RefId = string.IsNullOrEmpty(Request.Form["RefId"]) ? "0" : Request.Form["RefId"].ToString();
                 gg = "oooooo";
            }
            var str=MellatReturn(SaleReferenceId, ResCode, SaleOrderId, RefId);
            ViewBag.temp = SaleReferenceId + "--" + ResCode + "--" + SaleOrderId + "--" + RefId+"--"+str+"--"+gg;
            return RedirectToAction("ShowMsg", "Home", new { msg = ViewBag.temp });

Prameters like 'RefId','SaleReferenceId','SaleOrderId','ResCode' after using HTTPS missing but when using HTTp all of them has value. where is my mistake?


text:
Moore: Diamondbacks' Torey Lovullo has a lot on his mind ahead of wild-card game
Greg Moore
It was two days before the only game that matters, the winner-take-all National League wild-card matchup against the division-rival Colorado Rockies, and Diamondbacks manager Torey Lovullo had a lot on his mind.
His players were entertaining a small throng of reporters in the clubhouse Monday afternoon, mostly by giving variations of the same answer: "You have to treat this like a normal game, even though it's special."
Lovullo, meanwhile, was pondering roster moves. He wants to make sure it's "complete for a couple of different scenarios that maybe don't pop up during the course of the year.
"That's what we've been working on the past couple of days."
He is looking for an edge against a 6-foot-4, power-pitching, worst-case scenario in Rockies right-hander Jon Gray. Lovullo will have help from the Diamondbacks front office and analytics department, but he's going to be the one in the dugout with the season on the line Wednesday.
He knows as well as anyone that a feel-good, turnaround story of a first-time manager who helped mold a roster full of guys who lost 93 games one season into a swaggering bunch that won 93 the next could crash into a pile of what-ifs and why-nots if Gray has his best stuff.
Back in June, when the Diamondbacks, Rockies and Dodgers were setting a pace that was establishing the NL West as baseball's best division, Gray came off the disabled list to beat the Diamondbacks behind 10 strikeouts against one walk over six innings.
Paul Goldschmidt went 0 for 5 with three strikeouts that day. Typical. Gray owns Goldy. Arizona's MVP candidate is hitless in 11 career at-bats with five strikeouts against the Rockies ace. Goldschmidt hasn't been able to draw as much as a walk against Gray. But, hey, with Goldschmidt ending the season in an 0-for-17 skid, it's not like it can get worse.
The slumping superstar isn't the only one to struggle against Gray, though. Behind a 96-mph fastball and a 90-mph slider, the long-haired laser baller has gone 2-0 with a 2.77 ERA and 20 strikeouts to one walk in 13 innings at Chase Field this season.
One move could be at shortstop. Ketel Marte, 2 for 6 against Gray, tweaked his hamstring hustling out an infield single with the Diamondbacks up big in a statistically meaningless game on the last day of the season.
Lovullo couldn't be worried about criticism for having Marte in there competing that hard. The decision had already been made to play all-out to the finish regardless of whether anything was at stake. The danger of going into the postseason cold was far greater than the risk of a fluky injury. Hindsight wouldn't change that.
Marte said in the clubhouse Monday that he expected to play and would be "about 80 percent" by Wednesday, so Lovullo will pencil him in.
But what about Chris Owings? He's had plenty of success against Gray: 5 for 9 with a homer, a double and three RBIs. But Owings is trying to come back from the broken finger that gave Marte a spot in the lineup in the first place. He's close, but is he ready?
"I know that we're trying to figure if (Owings) is a possibility for Wednesday," Lovullo said. "I don't want to say it's a definite no, but I want him to continue working hard with the thought of making something special happen."
And what about catcher? It looks like Zack Greinke's personal valet, Jeff Mathis, seems ready to come back from a broken hand, suffered in August.
Mathis isn't the hitter Chris Iannetta is. He's better defensively, but not by much. This will come down to intangibles.
"We want to prioritize the potential for stopping the opposition," Lovullo said. "So, in my mind, pitching and defense is what wins you championships, and in this game, it's been my experience that every moment matters. Somebody gets on base, it's like red alert. And you're very tense for nine innings. So, you're looking for the best strategy to work through and navigate on the mound."
Mathis and Greinke developed a bond through the first three-quarters of the year, and the Arizona ace needs to be as comfortable as possible.
Besides, Lovullo trusts his process. "Will I change my strategy? Probably not," he said. "It's worked all year long here. We made it this far. For me to change and do something totally different, it's really not my style. But I can assure you that, if I do, it will have a strategy, there will be a reason for it."
Aside from all that, Lovullo is thinking about what to say to his team. How to get everyone to relax and be normal, even though everybody knows that everything is different.
This game matters more.
"I want these guys to understand that something special is happening here," he said, adding later, "I'll tell them to embrace this. … This is the greatest time of the year. October baseball, long-sleeve baseball, is the absolute best, and I want these guys to experience it, embrace it, and remember it."
2017 DIAMONDBACKS: A complete game's worth of key moments
HOW TO WATCH:Arizona Diamondbacks vs. Colorado Rockies in NL wild-card game
MORE:Arizona Diamondbacks gearing up for wild-card experience
Reach Moore at gmoore@azcentral.com or 602-444-2236. Follow him at www.Twitter.com/WritingMoore.
Wednesday's game
Rockies at Diamondbacks
What: NL wild-card game.
Where: Chase Field (Roof hotline: 602-462-6262).
TV/radio info: TBS/KMVP-FM 98.7.

redpajama_set_name: RedPajamaCommonCrawl


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The IRD will issue Forms B.I.R. 56A and I.R. 56B to employers for filing the remuneration and pensions of their employees. These forms are required to be submitted within one month or penalty will be imposed. The IRD has published comprehensive explanatory note on these two forms.


text:
\section{Introduction}
\label{sec:intro}

A   class of close binary systems consisting of Roche-lobe filling hot subdwarfs with white dwarf (WD) companions has been recently identified thanks to   optical surveys devoted to the discovery of transient and variable sources \citep{kup20b}.
Hot subdwarfs (see \citealt{heb16}, for a review)  are low mass stars ($\sim$0.3--0.8 ${\rm M}_{\odot}$), spectrally classified as sdO or sdB based on their effective temperature above or below 38 kK, respectively.
They are believed to originate from the evolution of stars that have lost most of their envelopes during the red-giant phase.
One of the  possible mechanisms responsible for the loss of the massive hydrogen envelopes necessary to form hot subdwarfs, is non-conservative mass transfer in a binary.  This is observationally supported by the large number of hot subdwarfs, particularly of sdB type, found in close binary systems \citep{mor03,nap04}.
Evolutionary models  predict that most of the companions of sdB stars in systems with orbital periods shorter than $\sim$10 days should be either late type main sequence stars or WDs \citep{han02,han03}.

Hot subdwarfs with WD companions are particularly interesting  because  they might be among the progenitors of type Ia supernovae \citep{ibe94}  and some of the nearby systems with ultrashort orbital period are expected to be sources of gravitational waves  detectable by LISA \citep{kup18}.
Furthermore, the determination of the mass and evolutionary stage of the two components, as done, e.g., for KPD 0422+5421 \citep{oro99}, KPD 1930+2752 \citep{gei07},  and HD\,49798\ \citep{mer09}, can shed light on the poorly known processes that take place during the common-envelope evolutionary phase.

The hot subdwarfs with WD companions that exit the common-envelope phase at orbital periods $P_{\rm orb}\lsim2$ hr will reach contact while the sdB is still burning He \citep{bau21}. Due to the emission of gravitational waves, the orbit will shrink until the sdB star fills its Roche-lobe at an orbital period  dependent on the evolutionary stage of the subdwarf
\citep{ibe91,yun08}.
The known population of sdB binaries consists mostly of systems with orbital periods too large to start accretion before the sdB turns into a WD \citep{kup15}.
Until recently, only five binaries of this kind with  $P_{\rm orb}$\lower.5ex\hbox{\ltsima}\ 2 hr were known \citep{ven12,kup17a,kup17b,pel21,kup22}.
The sdBs in these systems do not fill their  Roche-lobe.  X-ray observations of one of them (CD\, --30$^\circ$\,11223 , $P_{\rm orb}$=70 min) provided an upper limit on the X-ray luminosity indicating a wind mass-loss  rate  from the sdB star lower than  $\sim3\times10^{-13}$ ${\rm M}_{\odot}$ yr$^{-1}$  \citep{mer14}.

The first Roche-lobe filling subdwarf with a WD companion, ZTF\,J213056.71+442046.5\ (hereafter ZTF\,J2130 ,  \citealt{kup20}) was identified in a search for periodic objects in a  catalog of $\sim$ 40,000 hot subdwarf candidates  \citep{gei19} and first discovered in a dedicated high-cadence survey  with the Zwicky Transient Facility \citep{bel19}.
ZTF\,J2130\ consists of a sdB star  with mass $\sim0.35 {\rm M}_{\odot}$ and radius 0.13$\pm$0.1 $R_{\odot}$ and  a  WD of $\sim0.56 {\rm M}_{\odot}$.  The orbital period of this system, $P_{\rm orb}$ = 39 min (also independently discovered by G.~Murawski\footnote{https://www.aavso.org/vsx/index.php?view=detail.top\&oid=689728}),  is the shortest of any known hot subdwarf binary.
The radial velocity curve of ZTF\,J2130\ indicates a circular orbit with  a velocity semi-amplitude $K$ = 429 $\pm$ 28 km s$^{-1}$.  The periodic variability is primarily caused by the ellipsoidal modulation of the subdwarf, due to its tidal deformation under the gravitational influence of the  companion. However, the optical light-curve cannot be described with a simple model composed of two detached stars.

\citet{kup20} showed that the subdwarf in this system fills its Roche-lobe and the WD is surrounded by an optically thick accretion disk of size $\sim0.14 R_{\odot}$.  The formation of a disk is not surprising in a Roche-lobe filling system, and its presence suggests the  possible emission of accretion-powered  X-rays.  A short pointing (1 ks) carried out with the X-ray Telescope on the \emph{Neil Gehrels Swift Observatory} in 2019 did not detect X-rays \citep{riv19}, giving a flux upper limit of the order of a few 10$^{-13}$ erg cm$^{-2}$ s$^{-1}$.  Here we report on a much deeper observation of ZTF\,J2130\ obtained with the \emph{XMM-Newton}\ satellite.
In the following we use the source distance of 1.29$^{+0.06}_{-0.04}$ kpc, derived from  the Gaia EDR3 parallax  \citep{bai21}.

\section{Data analysis and results}
\label{sec:data analysis}

The field of ZTF\,J2130\ was observed  with  the \emph{XMM-Newton}\ satellite for about 65 ks starting at 23:47 UT of 2021 January 6.
We used the X-ray data obtained with the EPIC instrument, comprising one pn \citep{str01} and two  MOS cameras \citep{tur01} operating in the 0.2--12 keV energy range,  and with the Optical Monitor (OM,   \citealt{mas01}).
The three EPIC cameras were used in full frame mode  with the thin optical filter. The OM provided data in the  UVW1 band ($\lambda_{eff}$=291 nm, $\Delta\lambda$= 83 nm) for the first 26.4 ks and in the UVW2 band ($\lambda_{eff}$=212 nm, $\Delta\lambda$=50 nm ) for the remaining part of the observation.
All the data were processed with Version 19.0.0 of the Science Analysis Software (\textsc{sas})\footnote{https://xmm-tools.cosmos.esa.int/external/xmm\_user\_support/ documentation/sas\_usg/USG/}.

\subsection{  EPIC X-ray data}
\label{sec-epic}

The EPIC data were affected by periods of high background caused by  soft proton flares. Removing the corresponding time intervals
resulted  in  net exposure times  of 31 ks  for the pn and 37 ks for the MOS. We extracted images from the three cameras in five different energy ranges (0.2-0.5, 0.5-1, 1-2, 2-4.5, and 4.5-12 keV), both using the  cleaned data and the whole observation. Many sources were clearly visible in these images, but none  at the  position of ZTF\,J2130 .

We performed a more detailed analysis by  means of a source  detection procedure over the whole field of view using the data of the three cameras simultaneously.  This was done in the five energy bands given above using the SAS task \textsc{edetect\_chain}\footnote{https://xmm-tools.cosmos.esa.int/external/sas/current/ doc/edetect\_chain/index.html},
as described in the Appendix, and resulted in the detection of  51 sources (see Table~\ref{table-sources})
above a threshold likelihood $L$ = 10, corresponding to a confidence level of 99.9955 \%.
 ZTF\,J2130\ was not detected and we derived  an upper limit of 1.68 counts ks$^{-1}$ on its count rate in the 0.2-12 keV energy range (with a threshold likelihood $L$ = 8,  i.e. 99.97 \% confidence level).  The limits in the 0.2-0.5 and 0.5-4.5 keV ranges were 0.69 and 1.34 counts ks$^{-1}$, respectively.

\subsection{ OM ultraviolet  data}

ZTF\,J2130\ was clearly detected by the OM, with average count rates of 22 counts s$^{-1}$ in the UVW1  filter  (291 nm) and 2.5 counts s$^{-1}$ in the UVW2 filter (212 nm) (Table \ref{table:1}).   Figure~\ref{fig-lc} shows the OM light curves in the two filters folded at the orbital period according to the ephemeris of \citet{kup20}.
In both filters, the orbital modulation is consistent with that seen in the optical band, as it is shown by the superimposed solid lines representing the profiles obtained in the g-band with HiPERCAM \citep{kup20}.  Some small residuals remain.  These are most likely to be indicating factor of $\sim2$ variability in the accretion disc flux.

A search of periodicities was performed using the OM-UVW1 data, but the periodogram did not reveal any additional periodicity beyond the known orbital period of 39 min.

\begin{table*}
	\centering
	\caption{Ultraviolet and X-ray measurements of ZTF\,J2130\ obtained with \emph{XMM-Newton} . Errors in luminosity include the error in distance and are given at $1\sigma$. Magnitudes are not dereddened. The upper limit in the X-ray luminosity is valid for the blackbody and thermal bremsstrahlung models.
	}
	\label{table:1}
 \begin{tabular}{l c c c  c c r
		\hline
		Instrument & Band & $\lambda_{eff}$ & Exposure & Mean Magnitude & Flux & Luminosity\\
		           &      & (nm)           &(ks)       & (Vega)    & $\times 10^{-11}$ erg cm$^{-2}$ s$^{-1}$ & $\times10^{33}$ erg s$^{-1}$ \\
		\hline
		OM & $UVW1$     & 291  &   26.4 & $13.849 \pm 0.289$ & $3.16\pm0.84$    & $6.3\pm1.4$\\
		OM & $UVW2$     & 212	  & 37.32   & $13.809 \pm 0.003$ & $3.27\pm0.01$ & $6.51\pm 0.02$ \\
		EPIC   & 0.2-12 keV & --&31 (pn), 37 (MOS) &  --  & $<0.0012$ &  $<0.0025$\\
		\hline
	\end{tabular}
\end{table*}

\begin{figure}
    \centering
    \includegraphics[width=0.52\textwidth]{UV_OPT_02.pdf}
    \caption{The black points show the Optical Monitor light curves of ZTF\,J2130\ in two UV bands folded at the orbital period. The red  lines show for comparison the  g-band light curves.
    The second and fourth panels from top show the ratios between the UV and g-band light curves.
    The WD is between the observer and the sdB star at phase 0.5.}
    \label{fig-lc}
\end{figure}

\begin{figure}
    \centering
    \includegraphics[width=0.45\textwidth]{fig-UL_02.png}
     \caption{Upper limits on the luminosity of ZTF\,J2130\ as a function of temperature, for an assumed blackbody (red) or thermal bremsstrahlung (blue) spectrum. The solid and dashed lines give the unabsorbed luminosity in the 0.2-12 keV range for $N_{\rm H}$ = 1.7$\times10^{21}$ cm$^{-2}$ and 2.4$\times10^{21}$ cm$^{-2}$, respectively. The dotted lines give the bolometric (0.001-100 keV) unabsorbed luminosity for  $N_{\rm H}$ = 1.7$\times10^{21}$ cm$^{-2}$.  }
    \label{fig-ul}
\end{figure}

\section{Discussion} \label{sec:discussion}

Given the well known distance of ZTF\,J2130 , the most important factors affecting the conversion of the count rate upper limits derived in Section~\ref{sec-epic} to an upper limit on the luminosity are the spectral shape assumed for the X-ray emission  and  the amount of interstellar absorption.
Accreting  WDs have complex X-ray spectra, with different components depending on many   factors, including,  e.g., the WD mass and magnetic field, the geometry of the accretion flow, the binary orientation wrt the line of sight (see, e.g., \citealt{muk17}, for a review). Optically thin thermal emission originates from the shocked plasma, which in magnetic WDs is usually channeled in an accretion column. Depending on the plasma temperature, significant line emission can be present, in addition to the continuum bremsstrahlung flux.  Part of the emission from the accretion column can heat the star surface and will then be re-radiated as an optically thick soft thermal component.  Other spectral components can arise from Compton reflection of the hardest X-rays,  from the inner part of an accretion disk,   from the boundary layer, and from a hot corona above the disk.  Detailed models for many of these emission components have been developed, but for our purpose it is sufficient to adopt two simple models, blackbody and thermal bremsstrahlung,   which provide an adequate phenomenological description of the hard and soft components observed in accreting WDs.

 The 3-D extinction maps of \citet{gre19} give a reddening of $E(g-r)$=0.18 at the distance of ZTF\,J2130 . This corresponds to  $A_V\sim$0.6 mag, which, using the   relation between $A_V$ and  interstellar absorption   derived by \citet{bah15},   gives   $N_{\rm H}$=1.7$\times10^{21}$ cm$^{-2}$.
This value is consistent with the  upper limit provided by the total column density in this direction, $N_{\rm H}$=2.4$\times$10$^{21}$ cm$^{-2}$ \citep{HI4PI}.

Therefore, we computed the count rate to flux conversion factors for blackbody and   thermal bremsstrahlung models and two representative values of absorption (the nominal and the maximum values,  1.7 and 2.4 $\times10^{21}$ cm$^{-2}$, respectively). This was done using the response matrix for the EPIC instrument (i.e. the sum of the pn and two MOS) computed for the position of ZTF\,J2130\  in the instrument field of view.
The resulting upper limits on the luminosity are plotted as a function of the spectral temperature in Fig.~\ref{fig-ul}.  Except for the case of very soft spectral shapes, for which most of the emission falls outside the energy range sampled by the EPIC instrument, the limits are quite constraining and indicate a luminosity  below  $\sim10^{30}$ erg s$^{-1}$ for a wide range of assumed temperature values.

 By modeling the evolutionary history of ZTF\,J2130 , \citet{kup20} estimated that the WD in this system is accreting at a rate of  $\sim10^{-9}$ ${\rm M}_{\odot}$ yr$^{-1}$. Taken at face value, this would imply an accretion-powered luminosity of

\begin{equation}
L_{acc} =  G  \frac{M}{R}  \dot M = 5\times10^{33}  \dot M_{\rm -9}~~{\rm  erg~s^{-1}},
\end{equation}

\noindent
where G is the gravitational constant,  $\dot M_{\rm -9}$ is the mass accretion rate in units of 10$^{-9}$ ${\rm M}_{\odot}$ yr$^{-1}$, and we  used the   values of $M$=0.545 ${\rm M}_{\odot}$ and $R$=9400 km appropriate for this WD.
This luminosity is orders of magnitude larger than the upper limit derived with \emph{XMM-Newton} , but there are possible explanations for the lack of detectable X-ray emission in ZTF\,J2130 .

First, it must be considered that  about half of the accretion power is  dissipated in the accretion disk, which is too cold to emit in the X-ray band. Most of the disk luminosity occurs at IR/optical/UV wavelengths and  is outshined by the much brighter emission from the hot subdwarf present in this system. The latter has an effective temperature of 42,400 K and a bolometric luminosity of  41$\pm$9  $L_{\odot}$.
From the absence of optical emission lines, \citet{kup20} concluded that the accretion disk contributes at most 3\% of the overall luminosity, which is consistent with the above estimate of L$_{acc}$.

X-rays from accreting WDs can be emitted from the boundary layer between the disk and the star surface or,  in the case of intermediate polars, where  the magnetic field is sufficiently strong to channel the accretion flow, from  the shocked plasma in the accretion column. In this case, the maximum plasma temperature $T$ in the post shock region is an increasing function of the WD mass. A simple estimate  (e.g. \citealt{fra02}) is

\begin{equation}
T =   \frac{3}{8} \frac{G M \mu m_p}{k R },
\end{equation}

\noindent
which gives kT = 19  keV for ZTF\,J2130\
(m$_p$ is the proton mass and we used
a mean molecular weight $\mu$ =0.615).
Our luminosity upper limit for a thermal bremsstrahlung spectrum of this temperature is compared in Fig.~\ref{fig-IP} with the luminosities  of a sample of intermediate polars observed in the hard X-ray range \citep{sul19}. It is clear that, even if the mass accretion rate derived by \citet{kup20} were overestimated by up to a factor $\sim$100, the \emph{XMM-Newton}\ limit implies a   luminosity much lower than that of intermediate polars, that disfavors the presence of a magnetic WD in this system.

\begin{figure}
    \centering
    \includegraphics[width=0.5\textwidth]{Suleimanov_plot.png}
   \caption{Luminosity versus mass accretion rate in a sample of intermediate polars studied by \citet{sul19}. The values predicted by eq. (1) are shown by the blue and green lines for  M$_{WD}$=1 and 0.5 ${\rm M}_{\odot}$, respectively. The red line shows the upper limit we derived on the X-ray luminosity of ZTF\,J2130 . }
    \label{fig-IP}
\end{figure}

If the WD in ZTF\,J2130\ has a low magnetic field, the  available accretion power is mainly released in the boundary layer between the disk and the star, which might   be optically thick, and from the heated WD surface. The resulting  spectrum would peak at  soft X-ray/EUV energies  and  thus escape detection in the energy range covered by the  EPIC instrument.
Considering the high inclination of this system, it is also possible that the  emitting region is occulted by the accretion disk. In this respect, it is interesting to note the anticorrelation between soft X-ray luminosity and inclination found in non-magnetic cataclysmic variables by \citet{van96}.

Finally, we note the possibility that the  accretion rate derived   from the  evolutionary model used by \citet{kup20} has been overestimated.  An evolutionary phase with accretion rate at $\sim10^{-9}$ ${\rm M}_{\odot}$ yr$^{-1}$   is required to explain the current properties of this system, but it is possible that this phase is now ending and the sdOB has already started to  shrink and underfill the Roche lobe.

\section{Conclusions} \label{sect:conclusions}

ZTF\,J2130\ is the WD with a hot subdwarf binary companion with the shortest known orbital  period. The evidence, derived from optical observations, for an accretion disk around the WD, caused by Roche-lobe overflow of its sdB companion, motivated a search for X-ray emission.

Our \emph{XMM-Newton}\  observation, despite reaching a flux limit more than two orders of magnitude below the previously available one, could not reveal X-ray emission. The luminosity upper limit is in the range $\sim$(0.5--2.5)$\times10^{30}$ erg s$^{-1}$,  depending on the assumed spectral  temperature. For the hard Bremsstrahlung spectra typical of accreting magnetic WDs, this limit is significantly below the luminosity expected from the mass accretion rate of  $\sim10^{-9}$ ${\rm M}_{\odot}$ yr$^{-1}$ deduced from the evolution model of this binary.
This suggests that   ZTF\,J2130\  contains a non-magnetic WD,  that can have a luminosity up to a few $10^{33}$ erg s$^{-1}$, consistent with the theoretical accretion rate,  but characterized by a soft spectrum peaking in the EUV range and thus undetectable by  X-ray observatories. Alternative explanations for the lack of observable X-rays are either intrinsic absorption in the system, due to its  high inclination ($i$=86$^{\circ}$), or an overestimate of the current accretion rate implying that the Roche-lobe filling phase is nearly  ending.

\acknowledgments
We acknowledge  support via ASI/INAF Agreement n. 2019-35-HH and PRIN-MIUR 2017 UnIAM (Unifying Isolated and Accreting Magnetars, PI S.~Mereghetti).
TK acknowledges support from the National Science Foundation through grant AST \#2107982, from NASA through grant 80NSSC22K0338 and from STScI through grant HST-GO-16659.002-A.
TRM acknowledges support from the UK's Science and Technology Facilities Council (STFC), grant number ST/T000406/1.
This work is based on data obtained with {\it XMM-Newton}, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA).
This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.

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redpajama_set_name: RedPajamaArXiv


text:
La Serbia di Nedić (cirillico serbo: Недићева Србија, latino: Nedićeva Srbija) è il nome con cui era noto lo Stato serbo sotto l'occupazione militare della Germania nazista durante la Seconda guerra mondiale in seguito all'invasione della Jugoslavia.

Amministrazione

Lo Stato era guidato dal generale serbo Milan Nedić, sotto il comando militare tedesco e con il nome ufficiale di Vlada Nacionalnog Spasa (cirillico serbo:Влада Националног Спаса, italiano: Governo di Salvezza Nazionale), esistito tra il 1941 e il 1944. Geograficamente comprendeva la parte centrale della Serbia, la zona a nord del Kosovo (attorno a Kosovska Mitrovica), e la regione autonoma del Banato.

Incapace di resistere ai tedeschi, il generale Nedić consentì l'esistenza di campi di concentramento nel suo territorio, di una Gestapo serba, e di una legione Serbisches SS-Freiwilligen Korps.

Scioglimento
Con l'avanzata dell'Armata Rossa dalla Romania (che aveva abbandonato l'Asse e si era schierata con l'URSS nell'agosto del '44) verso i suoi confini, i tedeschi si ritirarono a nord-ovest per evitare l'accerchiamento, lasciando il governo di Nedić senza sostegno. Davanti alla prospettiva di essere egli stesso catturato fuggì in Slovenia (ancora sotto controllo tedesco) con tutto il suo governo. Molti serbi collaborazionisti furono catturati e giustiziati. I partigiani di Tito presero le redini della Serbia evitando che essa stessa fosse invasa dai sovietici col pretesto della liberazione; ciò permise, a fine conflitto, la costituzione di un regime socialista sotto la guida di Tito e indipendente dal Patto di Varsavia.

Voci correlate
 Bulgaria nella seconda guerra mondiale
 Stato Indipendente di Croazia
 Territorio del comandante militare in Serbia
 Campagna dei Balcani

Altri progetti

Stati costituiti negli anni 1940
Stati dissolti negli anni 1940
Storia della Serbia
Stati esistiti durante la seconda guerra mondiale
Jugoslavia nella seconda guerra mondiale

redpajama_set_name: RedPajamaWikipedia


Trained as a mechanical engineer not as a climate scientist, Harris previously was the executive director of the defunct Natural Resources Stewardship Project (NRSP), which shut down in 2008 after public revelations the group was controlled by energy industry lobbyists from the High Park Group.
Harris himself had been the Ottawa operations director of the High Park Group, a Toronto-based public policy and public relations firm specializing in energy industry clients like the transnational Areva nuclear power group, the Canadian Electricity Association, and the Canadian Gas Association.
For example, Harris and the ICSC last year promoted a skeptical climate change report produced by the Heartland Institute, identified by SourceWatch and others as a front for the ultra-conservative Koch Brothers, the primary backers of the Tea Party. Turns out that at least part of ICSC's funding and most of its key staff members come directly from the Heartland Institute.
The July 2011 edition of Nature magazine reported that the Heartland Institute "makes many bold assertions that are often questionable or misleading" with the goal is "muddying the waters" about the reality and importance of climate change, second-hand smoke hazards, and other ecology or health issues that invite government regulation.
The latest ploy in this PR strategy is a claim that climate change deniers are being frightened into silence. Reflecting this plan in his TGI commentary (submitted to many newspapers worldwide), Harris alleges death threats by environmentalists against Dr. Tim Ball, described as a "former climatology professor at the University of Winnipeg." Harris does not reveal that Dr. Ball today is a paid science policy advisor to oil companies along with being the past chairman of the NRSP, which Harris managed.
In his contention that environmentalists are dangerous, Harris is using the same propaganda trick being used here on Kauai to discredit the supporters of Bill 2491 (now Ordinance 960) by labeling peaceful citizen activists as "eco-terrorists" for wanting disclosure of the GMO seed-crop pesticides being sprayed almost daily on the island.
Among the tactics too often deployed to suppress evidence-based logic and critical thinking, the misleading irrationality and fear-mongering by Harris and ICSC smacks of the McCarthyism in the 1950s that repressed progressive post-war urges for social justice and open democracy. In the eyes of the climate change deniers, apparently, yesterday's reds are today's greens.
Let's praise news editors for publishing diverse views on public issues. Now let's do our part as readers to spot the fictions of propagandists posing as honest scientists.