text:
Bryan Anthony Smolinski, född 27 december 1971 i Toledo i Ohio, är en amerikansk ishockeyspelare  som har representerat NHL-klubbarna i Boston Bruins, Pittsburgh Penguins, New York Islanders, Los Angeles Kings, Ottawa Senators, Chicago Blackhawks, Vancouver Canucks och Montreal Canadiens. Han listades som den 21:e spelaren totalt i NHL-Draften 1990 av Boston Bruins.

Karriären i NHL
Efter att han spelat collegehockey i fyra år så anslöt Smolinski säsongen 1992/1993 till Boston Bruins, under den första säsongen skulle han bara spela 9 matcher. Men under säsongen därpå skulle han få spela 83 matcher och noterades för 31 mål och 51 poäng. Under året 1995 byte Boston bort Smolinski tillsammans med Glen Murray till Pittsburgh Penguins i utbytte mot Kevin Stevens och Shawn McEachern.

Smolinski tillbringade bara en säsong i Penguins men det blev en framgångsrik säsong. På 81 matcher gjorde han 24 mål och 64 poäng. Dock kunde inte Smolinski och Penguins enas om ett nytt kontrakt under försäsongen 1996/1997. Det resulterade i att Smolinski startade säsongen med att spela för Detroit Vipers i IHL. I november 1996 valde till slut Pittsburgh Penguins att byta bort Smolinski till New York Islanders mot backen Darius Kasparaitis och rookien Andreas Johansson.

I Islanders skulle han spela tre säsonger och det var säsongen 1996/1997 som var den bästa då han noterades för 28 mål och 56 poäng på 64 matcher. I juni 1999 skulle Smolinski ingå i en stortrade med Los Angeles Kings. Han själv skulle tillsammans med Žigmund Pálffy och målvakten Marcel Cousineau bli bortbytt mot spelarna Olli Jokinen, Josh Green och Mathieu Biron. Efter fyra stabila säsonger i Kings blev han återigen bortbytt, där har gången till Ottawa Senators.

Det blev bara två säsonger i Ottawa, under försäsongen 2006/2007 skulle han och Martin Havlát ingå i en trevägsdeal med Chicago Blackhawks och San Jose Sharks, där Smolinski och Havlat hamnade i Blackhawks. Men även den här gången skulle han få flytta på sig igen, efter 62 matcher valde Blackhawks att byta bort honom till Vancouver Canucks. Smolinski skulle spela ytterligare en säsong i NHL, under sommaren 2007 skrev han på ett kontrakt med Montreal Canadiens. I en match mot Boston skulle han spela sin 1000 NHL-match.

Efter NHL
Bryan Smolinski har egentligen inte annonserat att han har lagt av med hockeyn. Men han har inte spelat i NHL sen säsongen 2007/2008. Han har dock representerat IHL-laget Port Huron IceHawks och AHL-laget Milwaukee Admirals. Hans NHL-statistik står för tillfället på 1056 matcher, 274 mål, 377 assist och total 651 poäng. Han representerade total 8 NHL-klubbar.

NHL klubbar i karriären
Montreal Canadiens
Vancouver Canucks
Chicago Blackhawks
Ottawa Senators
Los Angeles Kings
New York Islanders
Pittsburgh Penguins
Boston Bruins

Spelare valda i NHL Entry Draft 1990
Amerikanska ishockeyspelare
Spelare i Boston Bruins
Spelare i Chicago Blackhawks
Spelare i Los Angeles Kings
Spelare i Montreal Canadiens
Spelare i New York Islanders
Spelare i Ottawa Senators
Spelare i Pittsburgh Penguins
Spelare i Vancouver Canucks
Spelare som har spelat minst 1000 matcher i National Hockey League
Personer från Toledo, Ohio
Födda 1971
Levande personer
Män
Ishockeyspelare i Michigan State Spartans
Alumner från Michigan State University
Spelare valda av Boston Bruins i NHL Entry Draft


PERUVIAN FOOD FOCUSES ON LOCAL INDIGENOUS INGREDIENTS: Ceviche Mixto garnished with Maitz Tostado—toasted corn nuts—and Fried Plantains, above.
Francoe Noriega is a celebrity chef based on somewhat humble beginnings as an underwear model. A Peruvian who has done a good bit of television, Franco, with the help of some PR, has become a celebrity Chef. Often wearing not much more than an apron, he is the owner of Baby Brasa, located on 7th Avenue and Perry Street in a glass building that had been a Chinese Restaurant for a long time. There is an original location in the East Village.
A CREATIVE CEVICHE: Salmon La Luz after being slightly seared tableside with a blow torch.
The restaurant has a young and colorful vibe about it with a bar when you walk in and many tables in almost a greenhouse type setting that was a bit chilly on a pre-March-snowstorm eve. The menu is a diversified sampling of Peruvian food which at times takes a gentle approach with broad appeal. Peruvian food focuses on local indigenous ingredients, often with a good bit of seafood and the best known example in the city is Nobu.
TRES LECHES. All photos by David Porat.
We started with Ceviche Mixto ($21), an assortment of raw seafood "cooked" in lemon vinaigrette. It was a fresh clean tasting plate that included a bit of sweet potato which added good flavor, texture and color. We also had the Salmon La Luz ($18) which is a more creative ceviche that included a mild pepper aioli with crispy quinoa, that was finished tableside with a blow torch to sear the fish and open up the flavor of the warmed sauce. For our main course we had the Lomo Saltado ($29) or a stir fry of sirloin strips with onions and tomatoes, served with both rice and french fries. This tasted a bit like Peruvian comfort food, the meat was tender and the sauce was good and maybe had an Asian vibe about it. We also had the Arroz con Pollo ($24) which was a quarter of the rotisserie dark meat chicken with cilantro rice, salsa criolla and papita huancaina. The latter two components include a fresh salsa, Peruvian style, and potatoes with a gentle yellow pepper sauce. The menu includes just the organic rotisserie chicken at modest prices which I have enjoyed before. We finished with Tres Leche cake which was very creamy and it was hard to resist chipping away at the generous piece. We also got an order of the Aalfajores or the dulce de leche filled shortbread.
We did overlook having a Pisco Sour, the popular Peruvian drink made with brandy from the pisco grape and citrus, that has a buzz about it—like Franco. I will have to go back for a drink and enjoy the lively and youthful atmosphere.


Questions regarding data and analysis for the purposes of use in the Petroleum Industry.
I am looking for oil and gas pipeline for Africa or Nigeria. I have tried searching the global energy observatory platform and I cannot find it.
I am looking for oil and gas pipeline data for the area near Parnaiba, Brazil. I've spent hours search the web and I have yet to locate a source. Does anyone have any suggestions?
Is there free pipeline shapefile data for Asia?
I need to find oil & gas pipeline data in the world especially about Asia but I want to get them freely.
I'm looking for free shapefiles of oil or natural gas pipelines pertaining specifically to Mexico or even trans-national pipelines between the U.S and Mexico.
Is there ArcGIS (ideally) solution for spill modeling from particular pour point on crude oil pipeline?
How to create a layer of directional/horizontal wells?
Parameters for ED50 -> ETRS89/WGS84 seven-parameter transformation which are good for Denmark?


text:
Q: Isolated Scope '=' passes a string instead of the object I'm trying to pass a model (Object) into the scope of the directive but it is passing a string instead of the object.
The directive html.
<blabla obj="obj"></blabla>

Directive:
.directive( 'blabla' , function(){
return {
    restrict : 'E',
    replace: 'true',
    scope :{
        obj : '=obj'
    },
    link : function(scope , elem , attrs){ console.log(attrs);
      scope.obj = attrs.obj;
    }
}})

Then in the controller I have:
$scope.obj = { name : "obj"};

And this is what I get in the console
obj: "obj"

Am I missing something? Why is it rendering 'obj' as a String instead of fetching the object? If I print the object on the page it works, but it doesn't work to pass it into the directive.

A: Don't use attrs.obj.
You should already have obj on the scope once the link function is run

redpajama_set_name: RedPajamaStackExchange


text:
As a prolific and masterful architect, Aalto is the undisputed doyen of Finnish, even Nordic, Modernism. First establishing his studio in the early 1920s, Aalto's architectural practice produced an eclectic oeuvre that spans the styles of Nordic Classicism, Functionalism and the International Style.
But to prescribe Aalto's projects as being examples of 'x' style is to deny the idiosyncratic architectural language he developed throughout his life. Like any true great, Aalto is considered as such because of his clarity of individual expression, uniqueness of design and uncharted experimentation.
Nowhere is that more evident than in his furniture, textile and lighting designs, of which the simple, almost naïve-looking '60 Stool' and the curvaceous 'Paimio Chair' – named after the tuberculosis sanatorium for which it was designed – are perhaps the most famous. They serve as perfect distillations of Aalto's greatest achievements: functionalist utility, bentwood innovation and sculptural elegance. ~ from The Modern House
Aalto's most important—and underappreciated—colleague was Aino Marsio-Aalto, his wife and professional partner. Alvar and Aino were such close collaborators that it is impossible to determine each individual's specific contributions to the work. The couple married and began their career partnership in 1924, and together oversaw the completion of significant projects like the Paimio Sanatorium and co-founded the furniture company Artek, which still sells their internationally acclaimed furniture. Were it not for Aino's untimely death from cancer in 1949, we would now likely privilege the couple over the individual and consider the Aaltos the Charles and Ray Eames of their day. ~ from The Architect Magazine
Model 901 Tea Trolley
Model 66 Chairs in Zebra Hide, pair
Armchair 41 "Paimio" Lounge Chair

redpajama_set_name: RedPajamaCommonCrawl


As you may already be aware, many of the newer online slot machines that have been released by some of the major slot game designers offer the new All Ways playing structure, when playing slots online at casinos that utilize the software engines from Microgaming, Playtech and IGT Interactive you will notice that some of them have been designed around this new payline type of structure.
The logic regarding the way these slots work is quite simple to understand, you may not understand the mathematics behind them, however in lay mans terms you will be forced to pay a set amount of credits to set any of these All Ways slots in live play, and by doing so all of the reel symbols and reel positions in view on each of their slot screens are active.
This means that as long as you get a winning combination as listed on the respective slots pay table in view consecutively from reel one onwards, then that winning combination is active and as such a winning payout will be awarded to you.
However as each slot has a different number of reel positions in view on each reel, then the actual winning paylines or ways to win that are activate is going to vary depending on which slot game you are playing, for example some slots offer 243 ways to win some can offer 1024 ways to win and a small collection of slots offer a massive 3125 ways to win.
Playtech have just launched the first in what is going to be a series of slots that instead of offering you just one set number of ways to win they will offer you the chance of playing one of these new slots with one of five different numbers of ways to win whenever you set the reels of the slot into live play.
One of the first slot games they have recently launched which offers this brand new Multiple All Ways playing structure is the Lucky Panda slot, and if you like playing slots on which you will have the maximum number of winning opportunities in play then this slot game is going to be well worth you checking out.
Fortunately when you are a member of any of our listed Playtech casino sites you can play the Lucky Panda slot game in the free play mode and this will let you put this new playing structure to the test for yourself, at no risk, and as such you will be able to quickly find out whether it is a structure you like and then may wish to play for real money.
There are as mentioned five different ways of playing the slot and as such we will now give you are quick rundown on how you can play it, depending on just how many ways to win you want to activate and put into play.
64 Ways to Win – The first way in which you can play the Lucky Panda slot game is by activating the 64 Ways to Win playing structure, this will see the first reel having all four of the visible reel positions activated on each spin you play, and the remaining four reels, those being reels 2, 3, 4 and 5 will only have the centre two reel positions activated when you play it via this structure. This playing format is going to cost you a total of 12 coins per spin you make.
128 Ways to Win – When you play the Lucky Panda slot game with its 128 Ways to Win playing structure activated then reels one and two will have all four of their visible reel positions activated and in play and the remaining reels those being reels 3, 4 and 5 will just have their middle two reel positions live and in play. The 128 ways to win playing structure will cost you an obligatory 24 coins per spin.
256 Ways to Win – For just 48 coins per spin you will be able to have a total of 256 ways to win in play on each spin of the Lucky Panda reels you make, however when playing in this format the first three reels will have all four of their visible reel positions live and activated and reels 4 and 5 will just have the middle two reel positions in play.
512 Ways to Win – For over 500 ways to win, in fact to be exact 512 ways to win when playing the Lucky Panda slot you will have to pay an obligatory 60 coins per spin and once you have chosen this playing format all of the first four reel symbols are fully activate and as such all four positions in view on each of their reels will be in play and on real five just the middle to positions on that reel are live and activated.
1024 Ways to Win – For the maximum chances of winning on every single spin of the Lucky Panda slot games reels you set in motion then you need to play with the 1024 ways to win playing structure in play. This will cost you a total of 72 coins per spin but by playing that amount of coins every single reel position on all five of its reels will be live and in play.
So when playing 1024 ways to win whenever you get three of any type of matching reel symbols spinning in and landing on reels one, two and three anywhere in view then you are guaranteed to win a cash payout, get the same matching symbols on reels four and five also then you will be awarded one of the higher winning payouts as listed on this games pay table.
If you do decide to play this Lucky Panda slot then if you can comfortably afford to do so make sure you play it with all 1024 ways to win in play, for this ensures you never miss out on a winning combination spinning in and also some of the better free spins bonus game payouts can be won when of course the free spins round is awarded.
We have recorded a video of the Lucky Panda slot machine and uploaded it on our Youtube channel so you can see what the game looks like. I've also embedded the video below for your convenience.


Whether you're looking for a fantastic Midlands based soul / R&B vocalist, a classy wedding band or a top class corporate function band, Soul Inspiration are the right choice for you! Wolverhampton based Soul Inspiration comprises of one of the West Midlands finest collection of contemporary musicians. The band delivers a fully live, soul, funk, Motown and RnB repertoire and play an array of material from classic soul to modern pop and with plenty of gospel flavour.
I just wanted to say a massive 'Thankyou' to you all for providing the music at our wedding, you were absolutely awesome! We were completely 'blown away' with how good the music sounded and we have had loads of people commenting on how good the band was. We have given your details to some of our friends that are getting married, so hopefully they will be in touch with you soon. Once again, thank you for all you did in making our day such an amazing one.
Soul Inspiration are a top drawer team of professional musicians, fronted by a dynamic lead vocalist, known for her silky smooth velvet tones. The band have honed their repertoire over the years in order to deliver a highly entertaining, foot stomping repertoire, full of classic hits from the likes of Aretha Franklin, Anita Baker, Randy Crawford, Gladys Knight and Michael Jackson (to name a few).
This amazing soul and Motown and R&B covers band is really something to be witnessed live. The musicians in the band come with well over 20 years of worldwide experience within the music industry, playing alongside and supporting artistes such as: Angie Stone, Eternal, Beverley Knight, Beyonce, Tunde, Prince, Bryan Adams, Roy Wood, Walsall Jazz Orchestra, Roy Hemmings, Drifters, Clem Curtis, Maxine Brown and Tommy Hunt.


As a Mom, I've realized just how important it is to nurture your MIND. Oh man, when you are not in the right mindset or you have things cluttering around in your head, Motherhood begins to seem so overwhelming and impossible. It is vital to our Mom Survival to ensure we stay in the right mindset not only when things are tough, but when things are good as well.
don't know if you've ever been frustrated sometimes with being a Mom. I'm in the season of having a 5 year old, 1 year old and another baby on the way. I'll soon have two young ones under 2 and it's terrifying.
Have you ever had one of those days when you just felt like the day would never end? Of course not, right!? You're a rockstar Mom and nothing fazes you! WRONG! Anyone can put on a happy face and pretend like everything in life is just peachy. I have definitely had many days where the countdown to bedtime started before breakfast.


text:
\section{Introduction}
It is well known that Einstein's theory of general relativity (GR) fails to give any concrete predictions around singularities due to the non-negligible quantum effects in the Planck regime.
Various attempts has been made to construct a consistent theory describing such a regime in the past decades. Among these theories, loop quantum gravity (LQG) presents a picture of granular and discrete space-time at Planck scale\cite{Ro04,Th07,As04,Ma07}. In this theory, it has been shown that the operators representing geometric observables (e.g., 2-surface area, 3-region volume, length of a curvature and integral of certain metric components) have a discrete spectra \cite{Ro04,Th07}. Namely, gravity in LQG is quantized. Because of the quantum features of the underlying spacetime geometry, LQG propose that singularities may not exist. This concept was first implemented precisely in the theory of loop quantum cosmology (LQC) which is constructed by applying the method of loop quantization to the homogeneous and isotropic cosmological model \cite{LQC5,Boj,Ash-view,AS11,BCM}. According to LQC, the classical big bang singularity is finally resolved by the quantum bounce scenario \cite{APS3,ACS}.

Beyond the big-bang singularity, another well-known type of singularities is inside the black holes. The simplest example is the Schwarzschild interior space-time. Because this region is isometric to the Kantowski-Sachs cosmological model, one can thus transport directly the techniques developed for homogeneous but anisotropic LQC. One can refer to \cite{AB06,Vandersloot07,Chiou08} for detailed predications of the model, where it was shown by solving the effective dynamics that the black-hole singularity can be resolved as expected. Moreover, these treatments differ by how to choose the quantum parameters introduced to quantize the Hamiltonian constraint in detail. Roughly speaking, these analyses can be classified as the following types. The first is the so-called $\mu_o$-type, where the quantum parameters us chosen to be a global constant on the phase space \cite{AB06}.   The second one is the so-called $\bar\mu$-type\cite{Vandersloot07,Chiou08}, where, in contract with the $\mu_o$-type, the quantum parameters are chosen to be a function on the phase space. Although the key result of singularity resolution holds in both of the two approaches, the detailed consequent effective dynamics differ from one to the other. Several physically undesirable results are caused. For example, in some approaches, the quantum replacement of the classical singularity could occur in the low curvature region \cite{AB06,M06,CGP08}; while in other approaches the quantum corrections to the classical spacetime are large near the black hole horizon which is expected to be the classical regime \cite{Vandersloot07,Chiou08}. By considering these weaknesses, one recently proposed a new scheme \cite{AOS1,AOS2}, which will be referred as the AOS approach below. The AOS approach can be regarded as an average of the $\mu_o$-type and $\bar\mu$-type approaches, where the quantum parameters are required to be a Dirac observable, that is, a function on the phase space which are constant along each dynamics trajectory but may vary from one to another. The AOS approach provides a new effective description of the macroscopic Kruskal extension of Schwarzschild black holes incorporating corrections due to quantum geometry effects of loop quantum gravity. This effective dynamics not only resolves the central singularity in the Planck region but also keep the classical regime such as the horizon unchanged.

With these achievements, the AOS approach certainly should be generalized to the other black hole background to test its universality, which is the purpose of the present work. To achieve this goal, we choose the Janis-Newman-Winicour (JNW) spacetime\cite{JNW,JNW1,JNW2,JNW3} for investigation in the present work. The JNW spacetime is a solution to the Einstein gravity minimally coupled to a massless scalar field which on one hand is more complicated than the Schwarzschild solution and, on the other hand, can reduce to the Schwarzschild case when the scalar field vanishes. In the JNW spacetime, beyond the central singularity as that in the Schwarzschild case, there also exists another singularity, called the naked singularity, which will be replaced by the horizon in the Schwarzschild case. The $\mubar$ scheme of such system has been studied in \cite{Chiou08b}. We utilize the Hamiltonian framework in order to study the quantum effective dynamics. The Hamiltonian constraint of this model is an addition of the gravity part and the matter part, of which the gravity part is the same as that for the Schwarzschild case. Thus for the quantum effective dynamics, we can just transport the one given in \cite{AOS2,Chiou08b} to our model as the gravity part of the effective Hamiltonian constraint and leave the matter part as the classical one, just like the usual treatment in LQC \cite{Ash-view}. The effective Hamilton's equations then can be obtained by assuming the quantum parameters in the effective Hamiltonian are Dirac observables. The solutions to these equations can be written down by using the elliptic integral and thus properties of the solutions can be analyzed analytically and numerically.
According to the results,  the quantum dynamics well agrees with the classical one in the classical region and the quantum correction coming out in the quantum region resolves the singularities. These achievements do not sensitively depend on the value of the quantum parameters.

 To study the quantum effective dynamics more precisely, the quantum parameters must be fixed. As mentioned above, we want to generalize the AOS approach to the current model. However, a direct generalization of the AOS approach, which transports directly the key equations used to solve the parameters to our case, leads to a problem that there do not exist any real quantum parameters making the consequent equations hold. Therefore, the generalization is highly non-trivial.
To solve this problem, we come up with new equations by balancing the physical interpretation of the quantum parameters and some other physical consideration. The consequent results of the new proposed equations can recover the AOS scheme when the matter part vanishes. It should be mentioned here that some previous studies on loop quantization of the JNW spacetime with $\mubar$ scheme can be found in \cite{Chiou08b}. These previous studies reveal that the quantum evolution of the JNW spacetime will involve a large number of numerical calculations and thus becomes an ideal arena to highlight our approach.

This paper is organized as follows. In section \ref{sec:two}, the Hamiltonian framework of the classical theory of the JNW spacetime is presented. By considering the classical dynamics, we finally select the region with low curvature to set the initial data of the quantum effective dynamics. In section \ref{sec:three}, the quantum effective dynamics is discussed with using the assumption  that the quantum parameters are the Dirac observables. In section \ref{sec:four}, we present our approach of how to constraint the quantum parameters and discuss some consequences. Finally, the present work is summarized in section \ref{sec:con}.

\section{Classical theory}\label{sec:two}

\subsection{Preliminaries}

Consider a massless scalar field $\varphi$ minimally coupled to gravity with GR, the action reads
\begin{equation}
S[g_{ab},\varphi]=\int \dd^4 x\sqrt{-g}\left(\frac{1}{2\kappa}R-\frac{1}{2}g^{ab}\nabla_a\varphi\nabla_b\varphi\right)
\end{equation}
where $\kappa=8\pi G$. Canonical analysis leads to
\begin{equation}
S[g_{ab},\varphi]=\int \dd t\int\dd^3x \left(\frac{1}{\kappa}\dot{A}_a^iE_i^a+\dot{\varphi}\pi_\varphi-G_i\Lambda^i-C_aN^a-CN\right)
\end{equation}
where
\begin{equation}\label{eq:Hamilc}
\begin{aligned}
G_i=&\partial_bE^b_i+\epsilon_{ij}^{\ \ k}A_a^jE^a_k\\
C_a=&\frac{1}{\kappa\gamma}E_j^bF^j_{ab}+\pi_\varphi\partial_a\varphi\\
C=&\frac{1}{2\kappa}\frac{E^a_iE^b_j}{\sqrt{q}}\epsilon^{ij}_{\ \ k}\left(F^k_{ab}-(1+\gamma^2)\epsilon^k_{\ mn}K_a^mK^n_b\right)+\frac{1}{2}\frac{\pi_\varphi^2}{\sqrt{q}}+\frac{1}{2}\sqrt{q}q^{ab}\partial_a\varphi\partial_b\varphi
\end{aligned}
\end{equation}
are the Gaussian, diffeomorphism and Hamiltonian constraints respectively. Here we used the Ashtekar-Barbero variables where it should be noticed that $E_i^a(x)$ and $\pi_\varphi(x)$ are densitied fields of weight 1.

At the classical level, a spherically static solution to such a system was obtained by Janis, Newmann and Winicor(JNW)\cite{JNW,JNW1,JNW2,JNW3}.
The usual JNW metric is given by
\begin{eqnarray}\label{eq:standardJNW}
\dd s^2=-\left(1-\frac{B}{r}\right)^\nu dt^2+\left(1-\frac{B}{r}\right)^{-\nu}dr^2+r^2\left(1-\frac{B}{r}\right)^{1-\nu}d\Omega^2
\end{eqnarray}
whereas the scalar field here reads \begin{eqnarray}
\varphi=\frac{q}{B\sqrt{4\pi}}\ln\left(1-\frac{B}{r}\right)
\end{eqnarray}
with $q^2$ being the scalar
charge. The two parameters $B$ and $\nu$ are given by\begin{eqnarray}
\nu=\frac{2m}{B}\\
B=2\sqrt{m^2+q^2}
\end{eqnarray}
with $m$ standing for the ADM mass. This solution recovers the Schwarzschild exterior spacetime by setting $\nu=1$. It should be noticed that in the JNW solution, $r$ cannot be smaller than $B$ and $r=B$ is a singularity for $\nu\neq 1$. However,  as inspired by the Schwarzschild interior metric, we can modified \eqref{eq:standardJNW} to be
\begin{equation}\label{eq:modifiedJNW}
\dd s^2=- \left(\frac{B}{\tau}-1\right)^{-\nu}\dd \tau^2+ \left(\frac{ B}{\tau}-1\right)^{\nu}\dd x^2+\left(\frac{B}{\tau}-1\right)^{1-\nu}\tau^2\dd\Omega^2
\end{equation}
with $\tau\in (0,B)$. It should be noticed that in \eqref{eq:modifiedJNW} the space and time coordinated exchange comparing with \eqref{eq:standardJNW}. The modified JNW metric \eqref{eq:modifiedJNW} gives us the Schwarzschild interior spacetime when the scalar field vanishes. It has two singularities, one locates at $r=B$ and the other is the center singularity at $r=0$. When it comes to the JNW spacetime below, we refer to the metric \eqref{eq:modifiedJNW}.

As in the interior of the Kruskal space-time, the homogeneous Cauchy slices $\Sigma$ of the JNW spacetime have topology $\mathbb{R}\times \mathbb{S}^2$. Thus we can introduce a fiducial metric $\mathring{q}_{ab}$ on $\Sigma$
\begin{equation}
\mathring{q}_{ab}\dd x^a\dd x^b=\dd x^2+r_o^2(\dd \theta^2+\sin^2\theta\dd\phi^2).
\end{equation}
where $x\in(-\infty,\infty)$, $\theta$ and $\phi$ are 2-sphere coordinates, and $r_o$ is a constant with dimensions of length. Since $\Sigma$ is non-compact in the direction $x$, we introduce an elementary  cell $\mathcal{C}\cong (0,L_0)\times \mathbb{S}^2$ in $\Sigma$ and restrict all integrals to this elemental cell to avoid the divergency problems of integrations.

Because of the symmetry, the scalar filed $\varphi$ is reduced to a constant and the fields $A_a^i(x)$, $E^a_i(x)$ and $\pi_\varphi(x)$ take the forms
\begin{equation}
\begin{aligned}
A_a^i\tau_i\dd x^a&=\frac{c}{L_0}\tau_3\dd x+b\tau_2\dd\theta-b\tau_1\sin\theta\dd\phi+\tau_3\cos\theta\dd\phi\\
E_i^a\tau^i\partial_a&=p_c\tau_3\sin\theta\partial_x+\frac{p_b}{L_0}\tau_2\sin\theta\partial_\theta-\frac{p_b}{L_0}\tau_1\partial_\phi\\
\pi_\varphi&=\frac{p_\varphi}{4\pi r_0^2L_0}\sqrt{\mathring{q}}
\end{aligned}
\end{equation}
The Poisson bracket of the phase space reads
\begin{equation}
\{c,p_c\}=2G\gamma,\ \{b,p_b\}=G\gamma,\ \{\varphi,p_\varphi\}=1.
\end{equation}
By employing the expression of connection and triad, the curvature $F$ of the connection $A$ and the extrinsic curvature $K$ take the forms
\begin{eqnarray}
F_{ab}^i\tau_i\dd x^a\dd x^b&=&\frac{bc}{L_0}\tau_1\dd\theta\wedge \dd x+\frac{bc\sin\theta}{L_0}\tau_2\dd\phi\wedge\dd x+(\sin\theta-b^2\sin\theta)\tau_3\dd\phi\wedge\dd\theta\label{Fterm}\\
\gamma K_a^i\tau_i\dd x^a&=&\frac{c}{L_0}\tau_3\dd x+b\tau_2\dd\theta-b\tau_1\sin\theta\dd\phi\label{Kterm}
\end{eqnarray}
where $\gamma$ is the Barbero-immirzi parameter. The constraints except the Hamiltonian in \eqref{eq:Hamilc} vanish automatically. Taking into account of Eqs.(\ref{Fterm}) and (\ref{Kterm}), the Hamiltonian constraint in \eqref{eq:Hamilc} is reduced to
\begin{equation}
C=-\frac{1}{2\kappa}\frac{1}{|p_b|\sqrt{|p_c|}}\frac{2 p_b  \left(\left(b^2+\gamma ^2\right) p_b+2 b c p_c\right)}{\gamma ^2 }\frac{\sin(\theta )}{L_0}+\frac{1}{2}\frac{p_\varphi^2L_0}{16\pi^2 |p_b|\sqrt{p_c}}\sin\theta
\end{equation}
which becomes
\begin{equation}
\begin{aligned}
H:=\int_{\mathcal C} N C=-\frac{1}{2G\gamma}  \left(\left(b+\frac{\gamma ^2}{b}\right) p_b+2  c p_c\right)+\frac{\gamma p_\varphi^2L_0^2}{8 \pi p_b b}
\end{aligned}
\end{equation}
after smeared by a lapse function
$$N=\gamma\sgn(p_b)\sqrt{|p_c|}b^{-1}.$$

\subsection{The classical dynamics}

As the hamiltonian smeared with lapse function $N=\gamma\sgn(p_b)\sqrt{|p_c|}b^{-1}$ does not admit analytical solutions, we introduce a new lapse function $\tilde N$ in order to found  analytical solutions, which reads
\begin{equation}
\tilde{N}=8\pi G \gamma bp_b N.
\end{equation}
This lapse function leads to a new smeared Hamiltonian constraint
\begin{equation}
\tilde{H}:=\int_{\mathcal C}\tilde NC=8\pi G \gamma bp_b H.
\end{equation}
Let $\tilde{t}$ be the corresponding time to $\tilde{H}$. Noting that $p_c c$ is a constant of motion, we could define $p_c c=:L_0\gamma m$. Then the Hamiltonian constraint can be factorized as
\begin{equation}
-8\pi G \gamma ^3 p_b^2=8 \pi  G \gamma \left(b p_b\right)^2+16 \pi  G\gamma^2 m L_0 \left(b p_b\right)-2G^2 \gamma ^3 L_0^2 p_{\varphi }^2=:\kappa\gamma(bp_b-y_+)(bp_b-y_-),
\end{equation}
where
\begin{equation}
y_\pm=-\gamma L_0 m\pm \gamma L_0\sqrt{m^2+\frac{Gp_\varphi^2}{4\pi}}.
\end{equation}
The Hamilton's equation of $bp_b$ leads to
\begin{equation}
\frac{\dd (bp_b)}{\dd \tilde{t}}=\{bp_b,\tilde{H}\}=-8\pi G \gamma^3 p_b^2=\kappa\gamma(b p_b-y_+)(b p_b-y_-).
\end{equation}
which, with denoting $y=bp_b$,  can give us
\begin{equation}
\begin{aligned}
y(\tilde t)&=y_-+\frac{y_+-y_-}{1+e^{\kappa\gamma (y_+-y_-)\tilde{t}}}\\
p_b(\tilde{t})^2&=-\frac{1}{8\pi G \gamma^3}\frac{\dd y}{\dd\tilde{t}}=\frac{(y_+-y_-)^2}{4\gamma^2}\cosh\left(\frac{\kappa\gamma}{2}(y_+-y_-)\tilde{t}\right)^{-2}\\
b(\tilde{t})&=\frac{ \gamma }{  \left(y_+-y_-\right) }\left(y_+e^{-\kappa\gamma  \frac{(y_+-y_2)}{2}\tilde{t}}+y_-e^{\kappa  \gamma\frac{(y_+-y_2)}{2}\tilde{t}} \right)
\end{aligned}
\end{equation}
Then,
 $p_c(\tilde{t})$ and $c(\tilde{t})$ are easy to be obtained as
\begin{equation}
\begin{aligned}
p_c(\tilde{t})=p_c^{(0)}e^{2T(\tilde{t})}\\
c(\tilde{t})=c^{(0)} e^{-2T(\tilde{t})}
\end{aligned}
\end{equation}
where
\begin{equation}
T(\tilde{t})= \kappa \gamma y_+\tilde{t}-\ln \left(e^{\kappa\gamma  \left(y_+-y_-\right)\tilde{t}}+1\right).
\end{equation}
By substituting the above solutions to the spherical metric
\begin{equation*}
\dd s^2=-\tilde{N}^2\dd \tilde{t}^2+\frac{p_b^2}{|p_c|L_0^2}\dd x^2+|p_c|\dd\Omega^2,
\end{equation*}
we have
\begin{equation}\label{eq:metricnonstandard}
\begin{aligned}
\dd s^2=&-\gamma ^2|p_c^{(0)}|L_0^2\frac{ \left(\frac{\left(y_+-y_-\right)}{\gamma L_0\tau}-1\right){}^{\frac{y_-+y_+}{y_+-y_-}}}{\left(y_+-y_-\right){}^2}\dd \tau^2+\frac{\left(y_+-y_-\right)^2 \left(\frac{ \left(y_+-y_-\right)}{\gamma L_0\tau}-1\right){}^{\frac{y_-+y_+}{y_--y_+}}}{\gamma ^2|p_c^{(0)}|L_0^2}\dd x^2\\
&+\frac{|p_c^{(0)}|\gamma ^2 L_0^2}{\left(y_--y_+\right){}^2}\left(\frac{ \left(y_+-y_-\right)}{\gamma L_0\tau}-1\right){}^{\frac{y_-+y_+}{y_+-y_-}+1}\tau^2\dd\Omega^2
\end{aligned}
\end{equation}
where we defined
\begin{equation}
 \tau:=-\frac{ \left(y_+-y_-\right) \tanh \left(\frac{\kappa\gamma}{2} \left(y_+-y_-\right)\tilde{t}\right)}{2 \gamma L_0}+\frac{y_+-y_-}{2\gamma L_0}.
\end{equation}
By comparing Eq.\eqref{eq:metricnonstandard} with the JNW metric \eqref{eq:modifiedJNW}
\begin{equation}
\dd s^2=- \left(\frac{B}{\tau}-1\right)^{-\nu}\dd \tau^2+ \left(\frac{ B}{\tau}-1\right)^{\nu}\dd x^2+\left(\frac{B}{\tau}-1\right)^{1-\nu}\tau^2\dd\Omega^2
\end{equation}
we can fix the parameters as
\begin{equation}
B:=\frac{y_+-y_-}{\gamma L_0}= 2\sqrt{m^2+\frac{Gp_\varphi^2}{4\pi}},\ p_c^{(0)}=B^2,\ -\nu=\frac{y_-+y_+}{y_+-y_-}=-\frac{2m}{B}.
\end{equation}
The solutions to the equations of motion can be rewritten with the variables $B$ and $\nu$  as
\begin{equation}\label{eq:classicalsolution}
\begin{aligned}
b(\tilde{t})&=\frac{ \gamma}{2}\left((1-\nu)e^{-\kappa\gamma^2 L_0 \frac{B}{2}\tilde{t}}-(1+\nu)e^{\kappa\gamma^2 L_0  \frac{B}{2}\tilde{t}} \right)\\
p_b(\tilde{t})^2&=\frac{B^2L_0^2}{4}\cosh\left(\kappa\gamma^2L_0\frac{B}{2}\tilde{t}\right)^{-2}\\
p_c(\tilde{t})&=B^2 e^{2T(\tilde{t})}\\
c(\tilde{t})&=\frac{\nu\gamma L_0}{2B}e^{-2T(\tilde{t})}\\
T(\tilde{t})&= \frac{1}{2}\kappa \gamma^2L_0  B(1-\nu )\tilde{t}-\ln \left(e^{\kappa\gamma^2 L_0B\tilde{t}}+1\right).
\end{aligned}
\end{equation}
It is not difficult to verify that $T(\tilde{t})+$constant is actually the time with respect to the lapse function $N$. However, $T(\tilde{t})$ is not monotonous with respect to $\tilde{t}$ if $\nu\neq 1$. Its monotonicity changes at
\begin{equation}
\tilde{t}_0=\frac{1 }{ \kappa\gamma^2L_0B}\ln(\frac{1-\nu}{1+\nu}).
\end{equation}
More precisely, $T(\tilde{t})$ increases when $\tilde{t}\in (-\infty,\tilde{t}_0)$ but decreases when $\tilde{t}\in (\tilde{t}_0,\infty)$. This property of $T(\tilde{t})$ tells us that $T$ cannot be a globally defined time coordinate. In other words, a chart with $T$ as its time coordinate cannot cover the entire JNW spacetime. The entire spacetime is divided into two parts from $\tilde t=\tilde t_0$ by $T$. In both of the two part, $T$ ranges from $-\infty$ to $T(\tilde t_0)$, namely, $T(\tilde t)\in(-\infty, T(\tilde t_0))$ in both of the two parts. However, different physical pictures are presented as $T\to -\infty$ in the two parts.
For the part where
$\tilde t\in (-\infty,\tilde t_0)$, $T\to -\infty$ leads to the naked singularity, while for the other part, $T\to -\infty$ presents the central singularity. For the Schwarzschild's case where $\nu=1$, the naked singularity is replaced by the horizon. Then $T(\tilde t)$ becomes a globally defined time coordinate of the interior Schwarzschild spacetime.

At the moment $\tilde t=\tilde t_0$, $T(\tilde{t})$ takes its maximal value
\begin{equation}
T(\tilde t_0)=\frac{1}{2}(1-\nu) \ln \left(\frac{1-\nu}{1+\nu}\right)-\ln \left(\frac{2}{1+\nu}\right).
\end{equation}
and $b(\tilde t_0)$ $c(\tilde t_0)$, $p_b(\tilde t_0)$ and  $p_c(\tilde t_0)$ read
\begin{equation}\label{eq:initialdata}
\begin{aligned}
b(\tilde t_0)&=0\\
c(\tilde t_0)&=\frac{2 \gamma L_0}{B}\frac{  \nu }{1- \nu ^2} \left(\frac{1-\nu}{1+\nu}\right)^{\nu }\\
p_b(\tilde t_0)&=\frac{1}{2} B L_0 \sqrt{1-\nu ^2}\\
p_c(\tilde t_0)&=\frac{1}{4} B^2 \left(1-\nu ^2\right) \left(\frac{1-\nu}{1+\nu }\right)^{-\nu }.
\end{aligned}
\end{equation}
The scalar curvature is
\begin{equation}\label{eq:classicalR}
R=-\frac{8 }{B^2 \left(1-\nu ^2\right)}\left(\frac{1-\nu }{1+\nu}\right)^{\nu }.
\end{equation}
which will be much smaller than $ 1$ for $B\gg 1$ and all of $0<\nu<1$. Thus around $\tilde t=\tilde t_0$ is a classically region. In other words, when $\tilde t=\tilde t_0$, the quantum correction should be tiny such that the quantum dynamics is compatible with the classical one. This guides us to initialize the quantum dynamics.

\section{Quantum theory}\label{sec:three}
We adopt the same convention in \cite{AOS1,AOS2}. Then the effective Hamiltonian of the JNW spacetime reads
\begin{eqnarray}
H_{\rm eff}=-\frac{1}{2G\gamma}\left[2\frac{\sin(\delta_c c)}{\delta_c}p_c+\left(\frac{\sin(\delta_b b)}{\delta_b}+\frac{\gamma^2\delta_b}{\sin(\delta_b b)}\right)p_b\right]+\frac{\gamma \delta_bp^2_\varphi L_0^2}{8\pi \sin(\delta_b b)p_b}
\end{eqnarray}
with
\begin{equation}
N=\gamma\sgn(p_b)\sqrt{|p_c|}\frac{\delta_b}{\sin(\delta_bb)}
\end{equation}

In the quantum theory, we choose the time coordinate with respect to same $N$, which corresponds to $T(\tilde t)$ of the classical theory define in \eqref{eq:classicalsolution}. This time coordinate in the quantum dynamics will be also denoted as $T$. Taking advantage of the choice of this time coordinate, we can solve the evolution of $p_c$ and $\tan(\delta_c c)$ analytically. By using the Hamilton's equations for $p_c$ and $ c$
\begin{eqnarray}
\frac{\dd p_c}{\dd T}&=&2p_c\cos(\delta_c c), \nonumber\\
\frac{\dd c}{\dd T}&=&-2\frac{\sin(\delta_c c)}{\delta_c},\nonumber\\
\end{eqnarray}
we have
\begin{eqnarray}
\tan(\frac{\delta_c c(T)}{2})&=&c^{(0)}e^{-2T}\\
p_c(T)&=&\pm\frac{\zeta}{2}  \left(\frac{e^{2 T}}{c_0}+c^{(0)} e^{-2 T}\right)
\end{eqnarray}
with $\zeta=p_c\sin(\delta_c c)$ being the constant of motion corresponding to $cp_c$ in the classical theory \footnote{It is noticed here that, we have assumed $\delta_c$ and $\delta_b$ are Dirac observables. The validity of such assumption can be confirmed by using the same strategy adapted in the Appendix A of \cite{AOS2}.}.  As discussed under \eqref{eq:initialdata}, we should set the initial data such that the quantum dynamics around $T=0$ is compatible with the classical one around $\tilde t=\tilde t_0$. This principle leads to
\begin{equation}
c^{(0)}=\frac{\gamma L_0\delta_c}{B}\frac{\nu}{1-\nu^2}\left(\frac{1-\nu}{1+\nu}\right)^\nu.
\end{equation}
and
\begin{equation}
\zeta=\delta_cL_0\gamma \frac{\nu B}{2}.
\end{equation}
Thus we have
\begin{equation}\label{eq:solutionpc}
\begin{aligned}
\tan  (\frac{\delta_c c}{2})&=\frac{\gamma  L_0 \delta _c}{B}\frac{\nu }{1-\nu ^2}\left(\frac{1-\nu}{1+\nu }\right)^{\nu }e^{-2 T}\\
p_c&=\frac{B^2}{4}(1-\nu ^2)\left(\frac{1-\nu}{1+\nu }\right)^{-\nu }\left(e^{2 T}+\frac{\left(\gamma  L_0 \delta _c\right)^2}{B^2}\frac{\nu ^2}{\left(1-\nu ^2\right)^2}\left(\frac{1-\nu}{1+\nu }\right)^{2 \nu }e^{-2 T}\right)
\end{aligned}
\end{equation}
which recovers the classical solution \eqref{eq:classicalsolution} if $\tan(\delta_cc/2)\ll 1$.

Let us denote $\cos(\delta_b b)=:\xi$ below for abbreviation. The Hamilton's equation for $\xi$ gives
\begin{equation}\label{eq:xidot}
\begin{aligned}
\frac{\dd \xi}{\dd T}&=\frac{1}{2} (1-\xi^2+\gamma^2\delta_b^2)+\frac{G\gamma ^2  \delta _b^2 p_{\varphi }^2L_0^2}{8\pi  p_b^2}
\end{aligned}
\end{equation}
By employing the constraint equation $H_{\rm eff}=0$, we get
\begin{equation}\label{eq:pbofxi}
\begin{aligned}
p_b^{(\pm)}
=\frac{ L_0m\gamma \delta_b \left(-\sgn(\sin(\delta_bb)) \nu\sqrt{1 -  \xi ^2}\pm \sqrt{(1-\nu^2) \gamma ^2 \delta_b^2+  \left(1-\xi ^2\right)}\right)}{ \nu\left(1-\xi^2+\gamma ^2 \delta_b^2\right)}.
\end{aligned}
\end{equation}
Substituting \eqref{eq:pbofxi} into \eqref{eq:xidot}, we have that
\begin{itemize}
\item for $\sgn(\sin(\delta_b b))>0$, the two solutions  $p_b^{(\pm)}$ read
\begin{equation}\label{eq:detail1}
\begin{aligned}
\frac{\dd T}{\dd \xi}
=\frac{1}{\gamma ^2 \delta_b^2-\xi ^2+1}\mp \frac{\nu(1 -  \xi ^2)}{\left(\gamma ^2 \delta_b^2-\xi ^2+1\right) \sqrt{(1-\nu^2)\gamma ^2 \delta_b^2+\left(1-\xi ^2\right)}\sqrt{1-\xi^2}}=:R_1(\xi)\mp R_2(\xi).
\end{aligned}
\end{equation}
\item for $\sgn(\sin(\delta_b b))<0$, the two solutions  $p_b^{(\pm)}$ read
\begin{equation}\label{eq:detail2}
\begin{aligned}
\frac{\dd T}{\dd \xi}
=\frac{1}{\gamma ^2 \delta_b^2-\xi ^2+1}\pm \frac{\nu(1 -  \xi ^2)}{\left(\gamma ^2 \delta_b^2-\xi ^2+1\right) \sqrt{(1-\nu^2)\gamma ^2 \delta_b^2+\left(1-\xi ^2\right)}\sqrt{1-\xi^2}}=:R_1(\xi)\pm R_2(\xi).
\end{aligned}
\end{equation}
\end{itemize}
Then
without loss of generality, we will define the functions $T^\pm (\xi)$ as solutions to
\begin{equation}\label{eq:dTpmdxi}
\frac{\dd T^\pm}{\dd \xi}=R_1(\xi)\mp R_2(\xi).
\end{equation}
More precisely, we have
\begin{equation}
\begin{aligned}
T^\pm(\xi)=\frac{-1}{2\sqrt{1+\gamma^2\delta_b^2}}\ln\left(\frac{\sqrt{1+\gamma^2\delta_b^2}-\xi}{\sqrt{1+\gamma^2\delta_b^2}+\xi}\,\frac{\sqrt{1+\gamma^2\delta_b^2}+1}{\sqrt{1+\gamma^2\delta_b^2}-1}\right)\mp \int_1^\xi R_2(\xi')\dd \xi'
\end{aligned}
\end{equation}
where the initial condition $T(\xi=1)=0$ is considered because we want the quantum dynamics around $T=0$ to recover the classical one around $\tilde t=\tilde t_0$.  Then all information of the quantum effective dynamics is stored in the two functions $T^\pm(\xi)$.

The integration of $R_2$ above is actually a summation of the standard elliptic integrals, that is
\begin{equation}
\begin{aligned}
\int_1^\xi R_2(x)\dd x
=k\nu \Big(F(\arcsin(\xi)\,|\,k)-F(\pi/2\,|\,k)\Big)-k\nu(1+n)\Big(\Pi(n,\arcsin(\xi)\,|\,k)-\Pi(n,\pi/2,k)\Big)
\end{aligned}
\end{equation}
where $F(\theta\,|\,k)$ and $\Pi(n,\theta\,|\,k)$ are the first and the third kind of elliptic integrals (refer to Appendix \ref{app:ellip} for details) and the parameters $k$ and $n$ are defined as
\begin{equation}\label{eq:kn}
k^2=\frac{1}{1+(1-\nu^2)\gamma^2\delta_b^2},\ n=-\frac{1}{1+\gamma^2\delta_b^2}.
\end{equation}
Therefore, $T^\pm(\xi)$ takes the form
\begin{equation}\label{eq:Tofxisol}
T^\pm(\xi)=\frac{-1}{2\sqrt{1+\gamma^2\delta_b^2}}\ln\left(\frac{\sqrt{1+\gamma^2\delta_b^2}-\xi}{\sqrt{1+\gamma^2\delta_b^2}+\xi}\right)\mp k\nu F(\arcsin(\xi)\,|k)\pm k\nu(1+n)\Pi(n,\arcsin(\xi)|k)+T_0^\pm
\end{equation}
with
\begin{equation}\label{eq:initialT}
T_0^\pm=\frac{-1}{2\sqrt{1+\gamma^2\delta_b^2}}\ln\left(\frac{\sqrt{1+\gamma^2\delta_b^2}+1}{\sqrt{1+\gamma^2\delta_b^2}-1}\right)\pm k\nu F\left(\pi/2|k\right)\mp k\nu(1+n)\Pi(n,\pi/2|k).
\end{equation}
A numerical method to compute the elliptic integrals, and therefore to compute $T^\pm(\xi)$, is introduced in appendix \ref{app:ellip}.

Now we have two solutions $T^\pm(\xi)$ to the equation \eqref{eq:xidot}. The meaning of these two solutions is understood by the following discussion.
In the classical theory, the spacetime must be divided at least into two parts if $T(\tilde t)$ is chosen as a time coordinate. In one part $b\in (-\infty, 0)$ and in the other part $b\in (0,\infty)$. Therefore, the spacetime constructed from the quantum effective dynamics is expected to be a union of two sub-manifolds. In each sub-manifold, $T$ is a well defined time coordinate. However, $T$, as emphasized, cannot be defined globally on the entire spacetime. Additionally, in the sub-manifold corresponding to the classical one where $b\in  (-\infty, 0)$, $\sin(\delta_b b)$ is expected to be $\sin(\delta_b b)\in (-1,0)$, and in the other, $\sin(\delta_b b)\in (0,1)$. In other words, the sign of $\sin(\delta_b b)$ changes if we move from one sub-manifold to the other. Thus, according to \eqref{eq:pbofxi}, in order to keep the continuity of $p_b$ at the moment $T=0$, namely in the Cauchy surface of the spacetime where $\xi=1$ and where the two sub-manifold is glued, we must assign, saying, $p_b^{(+)}$ to both of the two sub-manifold. This leads to the fact that in one sub-manifold solution to \eqref{eq:xidot} is given by $T^+(\xi)$ while in the other, it is given by $T^-(\xi)$ (referring to \eqref{eq:detail1} and \eqref{eq:detail2}).  According to the above discussion, figure \ref{fig:realsol} gives a plot of the evolution of $\sin(\delta_b b)$ and $p_b$ as functions of $T$ derived from $T^\pm(\xi)$, where, as a comparison, the classical results of $\delta_b b(T)$ and $p_b(T)$ derived from \eqref{eq:classicalsolution} are also shown. According to the numerical results shown in the figure, the difference between the classical and quantum dynamics increases gradually as $b$ becomes larger and larger, and simultaneously $p_b$ becomes smaller and smaller. The decreases of $p_b$ in the two parts of the entire spacetime driven by the classical dynamics are both replaced in the quantum effective dynamics by a bounce, which indicates to us how the two singularities in the JNW spacetime is resolved. Additionally, by comparing with the classical dynamics, it can be easily concluded that $T^-(\xi)$, corresponding to $p_b^{(-)}$ in \eqref{eq:pbofxi}, resolves the central singularity and that $T^+(\xi)$, correspond to the naked singularity side.
\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{solution_pb_cosb}
\caption{Plots of the evolution of $\sin(\delta_b b)$ and $p_b$ as functions of $T$ derived from $T^\pm(\xi)$. As a comparison, the classical results of $\delta_b b(T)$ and $p_b(T)$ derived from \eqref{eq:classicalsolution} are also shown. The parameters are chosen to be
 $m=10^4$, $\nu=0.5$, $G=1=\hbar$, $\gamma=0.2375$, $L_0=1$ and $\delta_b=0.0340$ which is computed by \eqref{eq:deltab}. By comparing the quantum dynamics with the classical one, we conclude that $T^-(\xi)$, corresponding to $p_b^{(-)}$ in \eqref{eq:pbofxi}, resolves the central singularity and that $T^+(\xi)$, corresponds to the naked singularity side. }\label{fig:realsol}
\end{figure}

Finally, as $\xi\in [-1,1]$, the time coordinate $T$ ranges in a finite interval, namely $T^\pm(-1)\leq T\leq 0$ in the two charts respectively. It should be noticed that the consequent spacetime is geodesic incomplete. While how to extend this spacetime will be left as our further topic.

\section{The quantum parameters of $\delta_b$ and $\delta_c$}\label{sec:four}
As it is known, the quantum parameters $\delta_b$ and $\delta_c$ are introduced to regularize the curvature $F^i_{ab}(x)$, namely to express the $F_{ab}^i$ with holonomies \cite{Ash-view,AOS1}. More precisely,  taking $F_{\theta,\phi}^i\tau_i$ for instance, it is regularized as the following:
we first evaluate the ratio $(h_{\square(\theta,\phi)}-1)/\left({\rm Ar}(\square(\theta,\phi))\right)$ with $h_{\square(\theta,\phi)}$ being the holonomy around a closed rectangular plaquette $\square(\theta,\phi)$ within the $\theta$-$\phi$ 2-sphere enclosing an area ${\rm Ar}(\square(\theta,\phi))$, and then take the limit ${\rm Ar}(\square(\theta,\phi))\to 0$. Then by replacing the holonomy as an operator, the quantum operator $\hat F_{\theta\phi}^i\tau_i$  is given. However, by considering the underlying quantum geometry,  when defining the operator, we take the limit as $\square(\theta,\phi)$ shrinks to $\Delta$ with $\Delta$ being the area gap proposed by LQG\cite{Ash-view,AOS1}. In the same manner, operators corresponding to the other two non-vanished curvature components $F_{\phi,x}^i\tau_i$ and $F_{\theta,x}^i\tau_i$ are defined  by using holonomies along plaquette $\square(\phi,x)$ and $\square(\theta,x)$ in the $\phi-x$ and $\theta-x$ planes respectively. Finally we have
$$\hat F_{ab}^i\tau_i=\lim_{{\rm Ar}(\square(a,b))\to \Delta}\frac{1}{{\rm Ar}(\square(a,b))}(h_{\square_{ab}}-1)$$
where $\square_{ab}$ lies in the $a-b$ plane. In this procedure, the quantum parameter $\delta_b$ and $\delta_c$ are introduced, where $\delta_b$ is the ratio length of each link in the plaquette $\square(\theta,\phi)$  and $\delta_c$, the ratio length of the links along the $x$-direction in the plaquettes $\square(x,\theta)$ and $\square(x,\phi)$ in the fiducial cell $\mathcal C$.

Roughly speaking there are two strategies to choose the quantum parameters $\delta_b$ and $\delta_c$. The first one is the so-called $\mu_o$-type strategy, where the quantum parameters are chosen to be a global constant on the phase space such that the areas of the plaquettes measured with the fiducial metrics $\mathring{q}$ limit to $\Delta$, while, in contract with the $\mu_o$-type strategy, the second one, the so-called $\bar\mu$-type strategy, choose the quantum parameters to be a function on the phase space so that the areas measured with the physical metrics $q_{ab}$ limit to $\Delta$. In the Schwarzschild case, both of the two strategies are considered \cite{AB06,Vandersloot07,Chiou08}. However it is revealed that the consequent quantum dynamics has some physically undesirable results. To overcome the limitations, a new scheme  straddling between the $\mu_o$ and $\bar \mu$ schemes is introduced by \cite{AOS1,AOS2}. The idea is to define $\delta_b$ and $\delta_c$ as Dirac observables which keep constant along the quantum effective trajectories but may differ from one trajectory to another. This idea will be also adopted in the current paper.

The strategy in \cite{AOS1} to fix the Dirac observables $\delta_b$ and $\delta_c$ is to demand that the plaquette $\square(\theta,\phi)$ and $\square(\phi,x)$ enclose $\Delta$ physically when evaluated on the transition surface $\mathcal T$ with $\mathcal{T}$ being the space-like, 3-dimensional surface which replaces the classical singularity and glues the trapped and an anti trapped regions. By considering the physical meaning of the quantum parameters $\delta_b$ and $\delta_c$, the authors of  \cite{AOS1,AOS2} selected them by demanding that the two plaquettes within the $\theta-\phi$ 2-shperes and $\phi-x$ planes,  used to regularize the curvature $F_{ab}^i$, enclose the minimum area when evaluated in $\mathcal{T}$. However, we will see below that this requirement cannot be satisfied always for $\nu \neq 1$.

Let us denote $T_{\rm bnc}^{(b\pm)}$ as the moments when $p_b$ bounces, where the index $+$ corresponds to the bounce of $p_b$ resolving the naked singularity and the index $-$ represents the bounce resolving the central singularities respectively. Then according to \eqref{eq:pbofxi}, the area of $\square(\phi,x)$ evaluated in $T_{\rm bnc}^{(b\pm)}$ is
\begin{equation}\label{eq:arpx}
{\rm Ar}(\square(\phi,x))^\pm=2\pi \delta_b\delta_c|p_b|\Big|_{T=T_{\rm bnc}^{(b\pm)}}=2\pi \delta_b\delta_cL_0\frac{ B \gamma \delta_b( \sqrt{(1-\nu^2)\gamma^2\delta_b^2+1}\mp \nu)}{2(1-\gamma^2\delta_b^2)}\cong ( 1\mp \nu)\pi \gamma\delta_b^2\delta_cL_0B.
\end{equation}
 Similarly, let us denote $T_{\rm bnc}^{(c)}$ as the moment when $p_c$ bounces. The area of $\square(\theta,\phi)$ evaluated in $T_{\rm bnc}^{(c)}$ is
\begin{equation}\label{eq:artp}
{\rm Ar}(\square(\theta,\phi))=\left.4\pi \delta_b^2p_c\right|_{T=T_{\rm bnc}^{(c)}}=2\nu\pi \gamma\delta_b^2\delta_c L_0 B
\end{equation}
where \eqref{eq:solutionpc} has been used. As a consequence of \eqref{eq:arpx} and \eqref{eq:artp}, for $\nu=1$, the areas ${\rm Ar}(\square(\phi,x))^-$ and ${\rm Ar}(\square(\theta,\phi))$ can equal the area gap $\Delta$ simultaneously if and only if $T_{\rm bnc}^{(b)}=T_{\rm bnc}^{(c)}$ \footnote{Since the naked singularity disappears classically in this case, the value of ${\rm Ar}(\square(\phi,x))^+$ corresponding to the factor $1-\nu$ in \eqref{eq:arpx} disappears too, that is, ${\rm Ar}(\square(\phi,x))$ takes only ${\rm Ar}(\square(\phi,x))\Big|_{T=T_{\rm bnc}^{(b)}}\cong 2\pi\gamma \delta_b^2\delta_c L_0 B$. }. Actually that both ${\rm Ar}(\square(\phi,x))^-$ and ${\rm Ar}(\square(\theta,\phi))$ equal $\Delta$ is the requirement used in \cite{AOS2} to determine the quantum parameters. However, this requirement is invalid for the case when $\nu<1$. This can also be seen from the numerical calculation presented in the Appendix \ref{app:nogo}, where we show that the equations
\begin{equation}\label{eq:Aeq}
\begin{aligned}
2\pi \delta_b\delta_c|p_b|\Big|_{T=T_{\rm bnc}^{(c)}}&=\Delta\\
4\pi \delta_b^2p_c\Big|_{T=T_{\rm bnc}^{(c)}}&=\Delta,
\end{aligned}
\end{equation}
 will have no solution for $\nu$ smaller than 1. It should be remarked that in this equation, $p_b$ takes the value
 \begin{equation}
 |p_b|=\frac{ L_0m\gamma \delta_b \left(\nu\sqrt{1 -  \xi ^2}+ \sqrt{(1-\nu^2) \gamma ^2 \delta_b^2+  \left(1-\xi ^2\right)}\right)}{ \nu\left(1-\xi^2+\gamma ^2 \delta_b^2\right)}.
 \end{equation}
 with which Eq.(\ref{eq:Aeq}) can return to the equations introduced in \cite{AOS2} for $\nu=1$.

 The result that \eqref{eq:Aeq} has no solution is regarded to be physically desirable. Otherwise, the Ricci scalar curvature at $T=T_{\rm bnc}^{(c)}$, which is
\begin{equation*}
R\Big|_{T=T_{\rm bnc}^{(c)}}\cong\frac{\pi \left(\nu +1\right)^2 }{2\nu ^4\gamma^2}\frac{  \left(8{\rm Ar}(\square(\phi,x)) ^2 {\rm Ar}(\square(\phi,\theta)) \nu ^2+{\rm Ar}(\square(\phi,\theta))^3\right)}{ {\rm Ar}(\square(\phi,x))^4  }+o(\delta_b^2),
\end{equation*}
will increase to $\infty$ as $\nu$ decreases to $0$, which is contradictory to the
results indicated by LQC and the studies on loop quantized Schwarzschild interior spacetime, that loop quantum effect could lead to an upper bound to the scalar curvature \cite{Ash-view,AOS2}.

Now the problem on how to constraint the quantum parameters in the current model comes out. At first, because of the physical meaning of $\delta_b$ and $\delta_c$, the existence of the area gap proposed by LQG should be considered. However, it should be noticed that the existence of the area gap does not mean that any area in a spacetime cannot be smaller than $\Delta$. A typical counterexample is a null plaquette whose area always vanishes. This is actually the case for the plaquette  $\square(\phi,x)$ in the Schwarzschild spacetime when evaluated in the horizon. The situation is similar for the JNW spacetime considered in the current paper. When $\nu\cong 1$, in the surface $T=T_{\rm bnc}^{(b+)}$ where the bounce of $p_b$ to replace the naked singularity occurs, the metric will be almost degenerate along the $x$ direction and well behaved along the $\theta$ and $\phi$ directions. That is, the surface $T=T_{\rm bnc}^{(b+)}$ almost behaves as a horizon. Therefore, considering the limitation that the area of $\square(\phi,x)$ cannot be smaller than $\Delta$ when referring to the moment $T=T_{\rm bnc}^{(b+)}$ seems not to be that physically meaningful. Moreover, if we keep that ${\rm Ar}(\square(\phi,x))^-=\Delta$, it will lead to that ${\rm Ar}(\square(\theta,\phi))<\Delta$ which is unphysical. Therefore in the current paper, we choose the equation ${\rm Ar}(\square(\theta,\phi))=\Delta$ as one condition to determine the quantum parameters by considering the existence of the are gap.

Moreover, there have two quantum parameters $\delta_b$ and $\delta_c$, so we need two equations to completely fix them. The second equation we proposed is
\begin{equation}\label{eq:tbEqtc}
T_{\rm bnc}^{(b-)}=T_{\rm bnc}^{(c)}.
\end{equation}
which, as mentioned above, is automatically satisfied for the Schwarzschild case if one used the strategy in \cite{AOS1,AOS2}. Moreover, the equation \eqref{eq:tbEqtc} also means that the volume of the fiducial cell reaches its minimal in $T=T_{\rm bnc}^{(b+)}$ and, thus the energy density and the scalar curvature increase to their maximal at this moment. In summary, the quantum parameters will be determined by the equations
\begin{equation}\label{eq:mainequations}
\begin{aligned}
T_{\rm bnc}^{(b-)}&=T_{\rm bnc}^{(c)}\\
4\pi \delta_b^2p_c\Big|_{T_{\rm bnc}^{(c)}}&=\Delta.
\end{aligned}
\end{equation}

Now it comes to how to solve the proposed equations.
By employing the exact solutions of $c$ and $p_c$, we will obtain that
\begin{equation}\label{eq:tbc}
T_{\rm bnc}^{(c)}=\frac{1}{2} \ln \left( \left(\frac{1-\nu}{1+\nu }\right)^{\nu }\frac{  \nu }{1- \nu ^2}\frac{\gamma L_0 \delta_c}{B}\right).
\end{equation}
In addition, Eq.(\ref{eq:Tofxisol}) gives
\begin{equation}\label{eq:tbbpval}
T_{\rm bnc}^{(b-)}=\int_1^0 \frac{\dd T}{\dd \xi}\dd\xi=\frac{-1}{2}\sqrt{-n}\ln\left(\frac{\sqrt{-n}+1}{1-\sqrt{-n}}\right)+k\nu nR_F(1,1-k^2,0)-
\frac{k\nu n(1+n)}{3}R_J(1,1-k^2,0,1+n).
\end{equation}
In the equations \eqref{eq:tbc} and \eqref{eq:tbbpval}, we used the fact that
\begin{equation*}
\cos(\delta_c c)\Big|_{T=T_{\rm bnc}^{(c)}}=0=\cos(\delta_b b)\Big|_{T=T_{\rm bnc}^{(b-)}}.
\end{equation*}
The elliptic integrals in \eqref{eq:tbbpval} have been rewritten by using the Carlson's form \eqref{eq:carlsonform} whose relation with the Legendre forms is given in
\eqref{eq:relationce}. By using the assumption that $\delta_b\ll 1$ which leads to $1-k^2\ll1$ and $1+n\ll 1$, the asymptotic behavior of $T_{\rm bnc}^{(b)}$ can be derived by using the formula \eqref{eq:assRF} and \eqref{eq:assRJ}. The result is
\begin{equation}\label{eq:assTbb}
\begin{aligned}
T_{\rm bnc}^{(b-)}\cong\frac{-1}{2}\sqrt{-n}\ln\left(\frac{\sqrt{-n}+1}{1-\sqrt{-n}}\right)+k\nu n\ln\left(\frac{4}{\sqrt{1-k^2}}\right)-k\nu n\sqrt{\frac{n+1}{k^2+n}}\ln\left(\frac{\sqrt{(k^2+n)}+\sqrt{n+1}}{\sqrt{1-k^2}}\right)
\end{aligned}
\end{equation}
which leads to
\begin{equation}\label{eq:tbbformula}
\begin{aligned}
e^{T_{\rm bnc}^{(b-)}}&\cong\frac{1}{2^{2 \nu +1}} \frac{\sqrt{1+\nu}^{\,\nu +1}}{ \sqrt{1-\nu }^{\,1-\nu} }(\gamma\delta_b)^{1+\nu }.
\end{aligned}
\end{equation}
Then the equation \eqref{eq:tbEqtc} becomes
\begin{equation}\label{eq:deltac_deltab}
\begin{aligned}
\delta_c=\frac{B}{\gamma L_0}\frac{1- \nu ^2} {  \nu } \left(\frac{1-\nu}{1+\nu }\right)^{-\nu }e^{2T_{\rm bnc}^{(b-)}}\cong \frac{B}{\gamma L_0}\frac{1} {  \nu } \frac{1}{4^{\,2 \nu +1}} (\nu +1)^{\,2\nu +2}(\gamma\delta_b)^{\, 2\nu+2}
\end{aligned}
\end{equation}
Substituting this result \eqref{eq:deltac_deltab} into the second equation of \eqref{eq:mainequations} which more precisely is
\begin{equation}
{\rm Ar}(\square(\theta,\phi))=2\nu\pi\gamma\delta_b^2\delta_c L_0 B=\Delta
\end{equation}
we finally have that
\begin{equation}\label{eq:deltab}
\delta_b\cong \left(\frac{\sqrt{\Delta}  } {\sqrt{2\pi} \left(\frac{\nu +1}{2}\gamma\right)^{ \nu +1}\frac{B}{2^\nu} }\right)^{\frac{1}{ \nu +2}}.
\end{equation}
Meanwhile, $\delta_c$ takes
\begin{equation}\label{eq:deltac}
\begin{aligned}
  \delta_cL_0\cong \frac{1} {  \nu } \left(\left(\frac{(1+\nu)^2\Delta}{8\pi}\right)^{\frac{1+\nu}{\nu}} \frac{\gamma}{ 4 B}\right)^{\frac{\nu}{\nu+2}}
 \end{aligned}
\end{equation}

Several remarkable features of our results should be discussed. First,
these results of $\delta_b$ and $\delta_c$ will recover that in the Schwarzschild case given in \cite{AOS1,AOS2} for $\nu=1$. Moreover, for the area ${\rm Ar}(\square(\phi,x))$ of the plaquette $\square(\phi,x)$, we obtain that
\begin{equation}
\begin{aligned}
{\rm Ar}(\square(\phi,x))&=2\pi \delta_b\delta_c|p_b|\Big|_{\mathcal T}=   \frac{\nu+1}{2\nu}  \Delta\geq \Delta.
\end{aligned}
\end{equation}
where the equality can be achieved only for $\nu=1$.

Secondly, the equation \eqref{eq:deltac} tells us that $\delta_c L_0$ is inversely proportional to  $\nu$, which means that $\delta_c$ can be very large for small $\nu$ if $L_0$ is fixed. This is incompatible  with the usual assumption that the quantum parameters take small values so that the quantum dynamics can be compatible with the classical ones in the classical regions.
However, in the current work such an assumption for $\delta_c$ is actually not necessary.
First of all, in the above derivation, we only assume that $\delta_b$ takes small value, which is coincide with the finally result \eqref{eq:deltab}.
Secondly, because the $x$-direction is the non-compact direction of the Cauchy surface, the link along the $x$-direction in the plaquettes $\square(x,\theta)$ and $\square(x,\phi)$ can be chosen with an arbitrary length. Therefore, $\delta_c$ can be arbitrarily large, with recalling that $\delta_c L_0$ is the length of our link with respect to the fiducial metric $\mathring{q}_{ab}$.
Moreover, the quantum dynamics actually can recover the classical one in the classical regions even though the parameter $\delta_c$ is large. Substituting the value of $\delta_c$ in \eqref{eq:deltac} into \eqref{eq:solutionpc}, we get that $\tan(\delta_c c/2)\ll 1$ around $T=0$.
Then in the classical region where $T\ll 1$,
 $$\frac{\delta_c c}{2}=\arctan\left( \tan(\frac{\delta_c c}{2})\right)\cong  \tan(\frac{\delta_c c}{2}),$$
  which gives a coincide result $c(T)$ with the classical solution $c(\tilde t)$ given in \eqref{eq:classicalsolution}. It should be reminded here that the time coordinate $T$ used in the quantum theory is the same as the function $T(\tilde t)$ up to a constant. In addition, the coincidence for $p_c$ can be verified easily by using the condition that $\delta_c L_0 \nu/B \ll 1$. Finally, since $\delta_b$ itself is small, the quantum and classical dynamics for $\delta_b$ and $p_b$ are compatible classically, which actually has been shown in Fig.  \ref{fig:realsol} as an example. Therefore, as a conclusion, large values of $\delta_c$ for small $\nu$ is not a problem in the sense that it will not lead to any incompatibility between the quantum and classical dynamics classically.

Finally, let us consider the evolution of the scalar curvature $R$. By definition of $R$ and the Hamilton's equation, the scalar curvature can be expressed as
\begin{equation}\label{eq:curvature}
\begin{aligned}
R=&\frac{1}{32 \gamma ^2 \delta _b^2 p_b^4 p_c}\Big\{B^4 \gamma ^4 L_0^4 \left(\nu ^2-1\right)^2 \delta _b^4+8 B^2 \gamma ^2 L_0^2 \left(\nu ^2-1\right) \delta _b^2 p_b^2 \left(2 \xi  \cos \left(c \delta _c\right)+\xi ^2-1\right)\\
&+16 p_b^4 \left(-\gamma ^4 \delta _b^4-4 \gamma ^2 \left(\xi ^2-1\right) \delta _b^2+\left(\xi ^2-1\right) \left(4 \xi  \cos \left(c \delta _c\right)+2 \cos \left(2 c \delta _c\right)+\xi ^2-7\right)\right)\Big\}
\end{aligned}
\end{equation}
In principle, by using the Hamiltonian constraint and the fact that $p_c\sin(\delta_c c)=m\gamma L_0\delta_c$, the right hand side of the above equation can be reduced to a form with only $p_b$ and $p_c$ as arguments. This function will be denoted as $R(p_b,p_c)$ below.
A numerical result of $R$ with $\nu=0.5$ and $B=10^5$ is shown in Fig. \ref{fig:riemanncurvature}, where the classical results of $R$ are also presented as a comparison. As shown in the figure, the curvature $R$ is bounded throughout its evolution and there are two peaks which resolve the classical divergences resulted from the two classical singularities. It is remarkable that the quantum dynamics changes the sign of the curvature and the singularities with negatively infinity curvature are finally resolved by positive-valued curvature bounces.
Since $R(p_b,p_c)$ is a function with only $p_b$ and $p_c$ as arguments, one peak therefore occurs exactly at the moment $T=T_{\rm bnc}^{(b-)}$ when $p_b$ and $p_c$ bounce simultaneously.  At this moment the curvature reads
\begin{equation}
\begin{aligned}
R(T_{\rm bnc}^{(b-)})
=\frac{2 \nu  (\nu +2)+3}{ (\nu +1)^2}\frac{8 \pi}{\gamma ^2 \Delta  }+o(\delta_b^2)\leq \frac{24 \pi}{\gamma ^2 \Delta }.
\end{aligned}
\end{equation}
which is uniformly bounded.
\begin{figure}
\centering
\includegraphics[width=0.6\textwidth]{curvature}
\caption{Numerical results of the evolution of the scalar curvature $R$, for both of the classical and the quantum dynamics with $B=10^7$.  According to the result, the classical divergences as a consequence of the classical singularities is replaced by bouncing evolution of $R$. The quantum dynamics changes the sign of the curvature and the classical singularities with negatively infinity curvature is finally replaced by positive-valued curvature bounces. The parameter in this plot is chosen as $L_0=1=G=\hbar$, $\gamma=0.2375$, $\nu=0.5$ and $B=10^5$}\label{fig:riemanncurvature}
\end{figure}

\section{Discussion and outlook}\label{sec:con}
In the current paper, we investigate the classical and the effective quantum dynamics of JNW spacetime. The classical dynamics indicates to us where is the classical region of the JNW spacetime, so that the quantum dynamics can be initialized. The resulted quantum dynamics matches well with the classical one in the classical region. The quantum correction leads to a bouncing evolution for both of $p_b$ and $p_c$, which means that the classical singularities can be finally resolved by the quantum theory. These results do not sensitively depend on the value of the quantum parameters.

To understand the quantum dynamics more precisely, the quantum parameters $\delta_b$ and $\delta_c$ should be fixed. In order to constraint these two parameters, we apply the idea to solve $\delta_b$ and $\delta_c$ as Dirac observables. This idea has been implemented for the Schwarzschild case, especially by the work \cite{AOS1}. However, the key equations  introduced in this work to solve the quantum parameters cannot be transported directly to our case. Thus we propose two new equations \eqref{eq:mainequations} by balancing the physical interpretation of the parameters and other physical considerations. Taking advantage of the asymptotic formula of the elliptic integrals which appears in the solutions to the Hamilton's equation, we finally obtained the approximated formula of $\delta_b$ and $\delta_c$. Properties of the results are then discussed. First of all, the values of $\delta_b$ and $\delta_c$, for $\nu=1$, return to the results for the Schwarzschild case derived by the AOS approach. Secondly, the resulted value of $\delta_c$ can be very large for small values of $\nu$, this seems to be contradictory to the usual perception that the quantum parameter should be small. However, according to our discuss, the large value of $\delta_c$ will not be a problem in the current work.

Finally, in spite of the above achievements, especially the proposal to solve the quantum parameters, there are still many attractive topics needing our further investigation. Among these topics, the most interesting one is on the extension of the resulting effective quantum spacetime. Since the integral curves of the vector filed $\frac{1}{N}\partial_T$ are geodesics with affine parameter, we can easily verify that the effective quantum spacetime with the time coordinate $T$ takes values such that $\cos(\delta_b b)\in (-1,1)$ is geodesic incomplete. It is then interesting to come up with the questions that what structures will be constructed for the maximally extended quantum spacetime and what kinds of physics will be obtained from that spacetime. All of these will be leave for our further works.

\begin{acknowledgements}
This work is supported by NSFC with No.11775082 and National Science Center (Poland) Sheng1, 2018/30/Q/ST2/00811

\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


I am an American like many other Americans, born into a family of mixed European and Native American ancestry. My interest in my own origins started early. I knew that my European ancestors were pagans who were converted to Abrahamic faiths, and that my Native ancestors were pagans mostly obliterated by those Europeans. I knew all of this in my childhood, and it led me to question the Christianity taught to me by my grandmother (a saintly woman who taught me to pray and seek the divine).
I read books, lots of books, on ancient Greek, Roman and Celtic religious traditions. I traced their roots eastward, into India, and began to read the Upanishads. Within Śrīla A.C. Bhaktivedanta Swami Prabhupāda's translation of Śrī Īśopaniṣad I saw a picture of Mahā-Viṣṇu reclining on the Causal Ocean emanating universes from his pores, and for me it was the moment when all the Western science I studied came together with all the complex imagery I had seen. The idea of a unified source and substance emanating all the manifold possibilities of material creation seemed a profound match for multiverse theory.
As I examined further I learned that Hinduism describes a unified reality, not the duality of creator and creation that I had been taught in Sunday school – and that this matched with the quantum physics I was reading about. All of the onerous Monotheistic dogma I had consumed by growing up in the United States was lifted from my shoulders, and instead of simply knowing that I didn't believe in Christianity, I realized that I had always intuitively inclined toward Hinduism. I now believe that we are all constituents of one ultimate consciousness as predicted by unified field theory, indestructible as predicted by the theory of the conservation of energy. I now believe in cyclic time – that universes are born and die repeatedly, rather than that creation is a one-off event moving along a linear timeline toward an ultimate judgment and everlasting reward or punishment.
I now believe that we are not separate from nature, but are a part of it – interacting with it on the level of consciousness – that it responds to our awareness and expectations as demonstrated by the collapse of light waves into particles when an observer is present. I no longer believe that mankind is born in utter depravity under the burden of original sin, but rather that we are part and parcel of the divine, sparks of the roaring fire of the Godhead, imbued with the same being, consciousness and bliss that emanated us. The Sanatana Dharma – the eternal, intrinsic nature of ultimate reality, has filled the cavities within me that were never addressed by a regimen of exclusive Truth and fear of Hell, and it has allowed me to accept the variety and harshness of the World by setting it within a wider perspective – that our lives are but a handful of dreams in a limitless sea of possibilities.


text:
Banks, Iain. COMPLICITY. [London]: Little, Brown and Company, [1993]. Octavo, boards. First edition. "COMPLICITY is certainly [Banks'] most horrific book. In this novel a Scottish eremite exacts horrible revenge on people who have committed crimes but got away with them; it is not a comfortable book, and is made even less so by its superficial construction as a work of detection. It is more difficult here, however, to sympathize with the central character who is a muckraking journalist, drug addict, and sexual masochist--his masochism is played off effectively against the murderer's sadism." - John Grant in Pringle (ed), St. James Guide to Horror, Ghost & Gothic Writers, ps. 33. A fine copy in fine dust jacket. (#164448).
See more items by Iain Banks
"First published in Great Britain by Little, Brown and Company 1993" on copyright page.


Aaron's rod among all the rods of the tribes only flourisheth.
Numbers 17:1 And the Lord spak to Moises, and seide, Speke thou to the sones of Israel, Numbers 17:2 and take thou yerdis, bi her kynredis, bi ech kynrede o yeerde, take thou of alle the princes of the lynagis twelue yerdis; and thou schalt write the name of each lynage aboue his yerde; Numbers 17:3 forsothe the name of Aaron schal be in the lynage of Leuy, and o yerde schal conteyne alle the meynees of hem. Numbers 17:4 And thou schalt putte tho yerdis in the tabernacle of boond of pees, bifor the witnessyng, where Y schal speke to thee; the yerde of hym schal buriowne, whom Y schal chese of hem; Numbers 17:5 and Y schal refreyne fro me the playnyngis of the sones of Israel, bi whiche thei grutchen ayens you.
Numbers 17:6 And Moyses spak to the sones of Israel; and alle princes yauen to hym yerdis, bi alle lynagis; and the yerdis weren twelue, without the yerde of Aaron. Numbers 17:7 And whanne Moises hadde put tho yerdis bifor the Lord, in the tabernacle of witnessyng, he yede ayen in the day suynge, Numbers 17:8 and founde that the yerde of Aaron, in the hows of Leuy, buriounnede; and whanne knoppis weren greet, the blossoms hadden broke out, whiche weren alargid in leeuys, and weren fourmed in to alemaundis. Numbers 17:9 Therfor Moyses brouyte forth alle the yerdis fro the siyt of the Lord to al the sones of Israel; and thei sien, and resseyueden ech his yerde.
It is left for a monument against the rebels.
Numbers 17:10 And the Lord seide to Moises, Bere ayen the yerde of Aaron in to the tabernacle of witnessyng, that it be kept there in to the signe of the rebel sones of Israel, and that her playntis reste fro me, lest thei dien. Numbers 17:11 And Moises dide, as the Lord comaundide. Numbers 17:12 Forsothe the sones of Israel seiden to Moises, Lo! we ben wastid, alle we perischiden; Numbers 17:13 who euer neiyeth to the tabernacle of the Lord, he dieth; whethir we schulen be doon awei alle til to deeth?


At BOLD Value, we help our clients address what are often the most pressing questions for their businesses -- those relating to growth, succession, and preservation. We do that by applying our Value Architecture for Growth and Succession methodology for the benefit of owners, executives, employees, family and the community.
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Over the last year I have been part of an international team designing and implementing a solar mini-grid village electrification project in Myanmar. Last month we visited four of the villages and presented a training program for the villagers to begin the process of educating them about the community owned power system they will soon be enjoying.
The most important thing about off-grid solar power systems is that they need to be understood as whole systems, with limited inputs and outputs. The solar panels put energy into the battery, the 'loads' (lights and appliances) drain it out. If there is not enough flowing in to keep up with the draining out, the battery will be emptied and the system will fail.
We use water to explain electricity because it flows in similar ways. The water in the bottle represents the energy stored in the a battery. The cups are solar panels, each providing what they can when they get re-filled by the Sun. Wooden stoppers represent switches that open up a flow of energy out of the battery.
Lead-Acid batteries should be fully recharged EVERY DAY when the Sun is shining. It is important to keep the flow of power OFF when it is not necessary! Let the cups of solar power flow in!
Village meeting under the shade tree at the monastery.
These systems will use pre-paid energy meters at every house to control consumer access. The solar PV systems are sized to provide a small amount of energy to each household every day for efficient lighting, phone charging and small electronics. To help ensure that consumers do not use more energy than the system can provide there will be 50 Watt power limiters at each consumer connection. This will prevent the villagers from using rice cookers, tea kettles and other high power consuming devices not appropriate for use with off-grid solar power systems.
Soon to be consumers of a solar powered mini-grid learn about energy efficiency.
The Sun fills the cups (solar panels) with energy. If dust covers the panels its like having a cloth over the cup, some of the flow is absorbed.
Wooden plugs are like switches, turning on consumer devices.
There is almost always a little leaking from the battery due to inefficiencies in the system. The worst culprit are inverters, devices that turn the direct current (DC) in the batteries into alternating current (AC) to distribute to the consumers.
LED lights are clearly the most efficient choice for lighting.
Tube lights look similar but can be very different in terms of power. LED tubes are best.
The plug in power meter shows how many Watts each device consumes.
Ingenious education presentation – I'm reminded of my NOLS classroom. Well done.
How are the micro grid projects progressing? I've listened in on your VivaTropical podcast interview with Josh and found your work very interesting.
My background is renewable energy and moving forward international micro grid development is on my radar.
Would like to discuss if you're available.


text:
Sky opens up, waterlogged Mumbai shuts down; traffic, train services hit – Times of India
Posted on September 24, 2020 Author Saraswati Comments Off on Sky opens up, waterlogged Mumbai shuts down; traffic, train services hit – Times of India
MUMBAI: Torrential rain drenched Mumbai and surrounding areas for the second day in a row on Wednesday. The BMC declared a holiday early in the day so that officegoers do not step out of their homes. However, as many areas went under, even those that were not chronic flood spots, vehicular traffic and local train services were affected.
The man in the street was surprised to witness such intense rain in September, and the India Meteorological Department's (IMD) statistics echoed this observation.
Multiple locations received an overwhelming 300mm of rain within a 24-hour span, Dharavi leading the scorecard with 341mm. Santacruz recorded 286.4mm, the season's highest single-day rainfall. IMD's Santacruz observatory recorded 381.3mm rainfall in the 36 hours ending Wednesday night.
A green alert of light to moderate rain has been issued for Thursday.
"After discussing the weather report with the IMD, I took clearance from the chief minister and chief secretary in the morning, to declare a holiday… so that officegoers don't face inconvenience…" said BMC chief Iqbal Chahal.
The night-long downpour caused waterlogging, leading to road closure and traffic disruption. The BEST had to divert a record number of 112 bus routes in 33 waterlogged locations. Thirty buses broke down. Train services were stalled through the day on the Harbour Line, while Central Railway resumed trains in phases till Thane by 7.45pm. Western Railway restored services to Virar after 4pm.
Some of the arterial roads that were submerged were the stretches outside Byculla police station, Oberoi Mall in Goregaon, JJ flyover, Minara Masjid junction, Dadar railway station, Bawla Compound, Gol Dewool, Wadi Port junction, Hindmata, Khetwadi, Girgaum, Alibhai Premji Marg, Sleater Road and Cotton Green. Andheri and Malad subways were closed for a time. Traffic along the Eastern Freeway was diverted even as vehicles were found abandoned on the Western Express Highway after being partially submerged.
Throughout Wednesday, civic authorities put their nose to the grind tackling natural and manmade challenges. A mudslide occurred on a hill slope near Hanging Garden, breaking the retaining wall of Khareghat Parsi Colony.
The BMC's overhead pipeline with its 'high-power pump' failed to work near the waterlogged Gandhi Market at King's Circle, exacerbating flooding in the area. Nair Hospital campus outside Mumbai Central station remained flooded for over 12 hours. "Covid-19 patients admitted in the tent outside had to be shifted to the hospital building early in the morning as the water levels were rising," said a doctor.
The Parsis of Avabai Kashinath Colony in nearby Tardeo were aghast to see their cars and motorcycles rapidly get submerged under deep water. "I have not witnessed such flooding since my childhood in the eighties, not even during the July 26, 2005 deluge. This is unprecedented," said a resident.
Neighbouring Thane and Navi Mumbai went under too. With 260mm average rainfall in 24 hours in Cidco and PCMC areas, low-lying locations in Navi Mumbai were waterlogged. Thane received 85.3mm rainfall in the 12-hour period till Wednesday night.
Source: https://timesofindia.indiatimes.com/city/mumbai/sky-opens-up-waterlogged-mumbai-shuts-down-traffic-train-services-hit/articleshow/78286744.cms
On CCTV, Man Attacked With Sword Near Mumbai Allegedly Over Trade Dispute – NDTV.com
The attack was captured by CCTV cameras in the neighbourhood Mumbai: A sword attack that left a man seriously injured has sparked tension at Vasai near Mumbai and prompted the police to launch a massive search for suspects. According to local residents, the attack could be a fallout of a dispute between two groups involved […]
Mumbai: From January, reach Virar hill temple in 3 minutes via cable-drawn rail – Times of India
Posted on November 23, 2020 Author Saraswati
MUMBAI: From January, devotees will be able to reach Jivdani temple, located on a hill in Virar, in just three minutes via passenger funicular rail service. A commissioning certificate for the funicular ropeway has been issued, paving wray for the final trials. Funicular rail, also known as inclined plane or cliff railway, is a type […]
Rap Artists From All Over Mumbai Battle It Out At Insaniyat's Rap Premier League Season 2 – mid-day.com
Rap Premier League is one of the most awaited Rap Battles of Mumbai where the best rap battlers compete against each other to win huge cash prizes. On the evening of 12th January 2023, over 16 rap artists and 150 spectators gathered at Subhedar Ramji Ambedkar Nagar, Worli to battle it out in the Season […]
Mumbai drenched – Mumbai Mirror
Mumbai rains live updates: Heavy rains, waterlogging throw normal life out of gear; suburban train services resume partially – Times of India


On March 17, 2014, the State Bank of Vietnam issued the Circular No. 06/2014/TT-NHNN providing for the maximum interest rate applicable to USD deposits of organizations, individuals at credit institutions.
Accordingly, credit Institutions; foreign bank branches shall apply interest rate applicable to USD deposits that is not higher than the maximum interest rate as announced by the Governor of the State Bank from time to time for deposits of entities (excluding credit institutions) and deposits of individuals.
Deposits shall include such forms as demand deposits, term deposits, savings deposits, deposit certificates, bills of exchange, bills, bonds and other forms of deposits received from entities (other than credit institutions), individuals.
The maximum interest rate applicable to deposits shall include payments for sale promotion in any form and be applied to the method of term-end interest payment and other methods of interest payment that are converted into the method of term-end interest payment.
Therefore, the maximum interest rate applicable to USD is 0.25% per annum for organization and 1.25% per annum for individual shall be annulled from March 18, 2014.
For interest rates applicable to term USD deposits of entities, individuals at credit institutions arising prior to March 18, 2014 shall be implemented until the expiry of the term; in the event where at the end of the agreed term, if the entities, individuals do not come for withdrawal, then the credit institutions shall apply interest rates for deposits in accordance with new provisions.
Credit institutions shall publicly post interest rates applicable to USD deposits at locations of deposit taking in accordance with provisions of the State Bank of Vietnam. It is strictly prohibited for credit institutions, in taking deposits, to offer sale promotion in any form (in cash, interest rate or other forms) that is contrary to provisions of applicable laws and of this Circular.
This Circular takes effects on March 18, 2014.


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Render - 2015 Mazda2
14/10/2013 - 11:01 | Mazda2, Mazda | Shrawan Raja
We can get a better look at the 2015 Mazda2 hatchback through a seemingly accurate rendering envisioned by a Japanese magazine a few months ago. We've shown you the same vehicle previously, but the latest scan uploaded by a user on Minkara isn't distorted or folded.
The new Mazda2 will debut next year (branded Mazda Demio in Japan) with an evolution of the KODO design language that we see on other Mazda family models such as the CX-5 and the CX-9. A shield-shaped radiator grille and slim headlamps form the front-end of the vehicle.
The 2015 Mazda2 shares the CX-5's platform and speaks the KODO design language.
Under the hood, expect the new SKYACTIV-G 1.5L 4cyl engine, tuned to output 100 HP. It would be matched to a 6-speed manual transmission or a new CVT.
The current Mazda2 shares its platform with the Ford Fiesta. However the next gen model is developed independently on the light-weight CX-5 platform which would also be used on successors of other Mazda cars. This triggers the possibility of the Mazdaspeed2 model with the CX-5's 2.0-liter or 2.4-liter engine, though there are no reports to back such a variant.
The new Mazda2 would be world premiered at one of the main motorshows, with New York and Paris likely contenders.
[Source - minkara.carview.co.jp]
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Last December, I ran across an artist that's I had never heard of before named, Sebastian Mikael and his brilliant new project, I C U U C ME, PT. 1. Immediately, he became one of my favorite artists due to his soulful vocals and his glaring similarities D'Angelo. Today, he drops off a dope new video for one of the EP's standouts, "DAD".
Shot at popular New York City venue, Baby's All Right and directed by Jonathan Riggs, the video is set to the backdrop of a real-life headlining show for Mikael and his band, which helps to drive home some of the more intimate lyrics in the song due to the venue's environment. Encouraging assistance from $ean Wire, Sebastian and Wire place the crowd in a trance with his high-pitched, incredibly impressive vocal range that is certainly one-of-a-kind.
With the follow up to I C U U C ME set to drop sometime this year, now would be a better time than ever to join the bandwagon. Watch the video below and see for yourself.


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Leslie Howard: Was "Gone with the Wind" star assassinated by the Nazis?
Actor and producer, Leslie Howard, disappeared on 1st June 1943 when the now infamous KLM Royal Dutch Airlines Flight 777, he was travelling in from Lisbon, Portugal to Bristol was attacked by the Luftwaffe over the Bay of Biscay, killing all seventeen on-board. The Germans are believed to have thought British Prime Minister Winston Churchill was on-board. Churchill was indeed in Algiers around that time and later wrote in his autobiography that a mistake was clearly made about his movements, which must have cost Howard his life. But, recent research suggests that Howard may have in fact been the target himself.
Howard had long been a thorn in the side of the Germans and had produced several propaganda films. It is thought that the true purpose of his trip to Portugal and Spain was to meet local propagandists and to bolster support for the Allies, while on a lecture tour organised by the British Council. News of his being on the flight was passed to Germans hours before it took-off.
At that time Howard's career was at an all time high. He had starred in many leading British and American films, including the 1939 Hollywood blockbuster Gone with the Wind with Clark Gable and Vivien Leigh, the 1941 anti-Nazi thriller "Pimpernel" Smith with Mary Morris and the 1942 British propaganda film The First of the Few with David Niven and Rosamund John, which told the tragic story of Spitfire designer RJ Mitchell.
David Niven, a friend of Howard, said that he was "…not what he seemed. He had the kind of distraught air that would make people want to mother him. Actually, he was about as naïve as General Motors. Busy little brain, always going."
The Times in London carried news of Howard's disappearance in the same edition that they reported the apparent death of Major William Martin, the subject of the 1956 film, The Man Who Never Was. The film starred Clifton Webb and Gloria Grahame and told the story of Operation Mincemeat, an idea drawn up by James Bond creator Ian Fleming, to drop a dead body off the Spanish coast dressed as an officer and with a briefcase handcuffed to one writs that included false documents pointing to an Allied invasion of Greece rather than Sicily. The body's identity was Major Martin and the announcement in The Times was a crucial part in the subterfuge plot.
Time magazine carried a story in its 14 June 1943 issue, which quoted the Dutch pilot's last radio message as, "I am being followed by strange aircraft. Putting on best speed. …we are being attacked. Cannon shells and tracers are going through the fuselage. Wave-hopping and doing my best."
Posted in Blog	disappearanceFlight 777Gone with the WindLeslie Howard
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I am Henry and thanks for checking out Old Quotes.
A little bit about me is that I am a huge history lover. I also have a love for reading and writing. I decided to create this blog as a way to follow my passion of writing and to share ideas, tips, advice, and general news with you.
I hope you enjoy my blog and feel free to connect!


Finish strong with tab and wafer sealing at Finishbinders. Tabs and wafers seal folded pieces and stitched products. Label Aire services are available to attach and add value to your printed project.
Think Finishbinders, Think Tab and Wafer Sealing.


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Why Adven
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Our model for tailor-made, long-term and brilliant partnerships.
Recovery of residues and waste streams
Food & Beverage industries
Pulp & Paper industries
Metal, Mineral & Mining industries
Chemical & Pharmaceutical industry
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Our model for long-term and brilliant partnerships.
Geoenergy based heating and cooling
New geoenergy solution in Mirka's factory cuts carbon dioxide emissions
Adven – News – New geoenergy solution in Mirka's factory cuts carbon dioxide emissions
News Real estates Geoenergy Hybrid energy solutions
Mirka and Adven have launched a new energy solution project in Mirka's factory in Jakobstad, Finland. Adven will implement an energy-efficient, low-emission hybrid energy solution for the current factory and its expansion under construction. The most important part of the solution is a new geofield. Mirka aims to reduce the factory's carbon dioxide emissions from energy use as much as possible.
A hybrid solution will be implemented at Mirka's site in Jakobstad. The key part of the solution is a new geofield. Geoenergy is solar energy stored in the soil, and it can be extracted from the bedrock or from the surface of the soil. It can be efficiently utilized for both heating and cooling buildings throughout the year.
In total, 115 geoenergywells, each 340 meters deep, will be drilled on the site. Also installed on the site will be two large air to water heat pumps, solar panels and a district heating system, which is needed during the harshest winter. Mirka's energy partner Adven will be responsible for designing, implementing and operating the energy solution.
The overall reduction in annual carbon dioxide emissions will be 900 tons, which is a significant change from the previous level.
"Our goal is to minimize the carbon dioxide emissions, and Adven will provide us with local green energy. Adven's expertise and the cooperation skills of their local staff make them an easy partner to work with," says Mirka's Project Office Manager Jari Lemberg.
The heat pumps will be used for cooling in the summer, when heat is stored in the geofield. In the winter, geoenergy and heat pump technology are used to heat the production plants.
Energy partners for more than two decades
Mirka has purchased energy as a service from Adven since the beginning of the 2000s. Currently, Adven is Mirka's energy partner in its factories in Jeppo and Oravais. This made it easy to choose Adven as the energy partner for the company's factory in Jakobstad, as well.
"The biggest reason for choosing Adven was their experience in completing projects under highly demanding conditions. We knew that this undertaking would be challenging. The existing factory is in operation and the new one is under construction at the same time as heat wells are being drilled, so space is running out on the plot," says Lemberg.
Lemberg says that the cooperation has gone smoothly. All the parties have been aware of each others' doings, and flexibility all around has ensured the least amount of disruption possible.
"Implementation has been technically challenging, as the work site was established quickly, and the factory is in operation during the whole time. Despite this, I believe that careful planning and seamless cooperation with Mirka and on the work site of the new expansion will help see the project through successfully," says Adven's Sales Manager Anssi Juvonen.
Mirka is constructing a new factory building to the southern end of its existing factory in Kvastberget, Jakobstad. The current factory facilities failed to meet the rapidly rising demand for electric sanders.
Quick facts about the energy solution:
Geofield: 115 wells, each 340 meters deep
Heat pumps 1,650 kW and air to water heat pumps 340 kW
Solar panels 100 kWp
Share of renewable energy 98%
Carbon dioxide emissions reduced by approximately 900 tons a year
The project will be implemented by the end of 2022
Our goal is to minimize the carbon dioxide emissions, and Adven will provide us with local green energy. Adven's expertise and the cooperation skills of their local staff make them an easy partner to work with.
Jari Lemberg
Mirka's Project Office Manager
Anssi Juvonen, anssi.juvonen@adven.com tel. +358 40 809 3160
Stefan Sjöberg, stefan.sjoberg@mirka.com tel. +358 40 824 7385
Mirka Oy
Mirka is an international company with 18 subsidiaries. 97% of net sales come from exports to more than 100 countries. Mirka specializes in flexible abrasives and products that allow for dust-free surface finishing. Mirka's advanced sanding and polishing machines provide outstanding benefits to users. Innovative machines and high-quality abrasives and products, polishing compounds and accessories give Mirka customers access to a complete sanding solution to meet their individual needs. Mirka aims to provide optimized surface treatment solutions for use before painting or other finishing processes. www.mirka.com
Once a month we send out a newsletter with a selection of the latest news and stories from our business areas and geographies.


After the Nuit Blanche in Paris in 2007, I have the pleasure to announce to you a light calligraphy show on Bellecour square during the Lyon Lights Festival .
For more information please consult on the program and selection (and detail of films please visit the festival's official website .
a project based on the interactivity of each individual with the universe. The visitor will be invited to interact with its contents to discover a new universe of which he/she will be a part.


Is MTV's 'Slednecks' Their Craziest Show Yet? Watch The Cast Take a Shot of Blood!
Forget the Jersey Shore — we're headed to Alaska!
MTV is ditching the bikinis and embracing the below-zero temperatures with their newest reality TV series Slednecks. Set in the rural town of Wasilla, Alaska (the same town that the Palins are from!) the half-hour comedy docu-series, follows a group of "outdoor tough" friends who use their hometown mountains and rivers as their playground.
According to MTV, the "Slednecks" are all about having fun and pushing their adventures to the extreme. Polar Bear plunges, airboating on ice, glacier parties, river wakeboarding, and human catapulting are just some of the outrageous activities this close-knit gang likes to do together.
NEWS: How to Dress Like the Most Badass Characters on TV!
To prove just how off-the-wall these teens are, we're snagged an exclusive sneak peek at one of the craziest scenes we've ever seen on MTV: The Slednecks cast taking a shot of blood together!
Okay to be fair, it's not human blood — it's caribou blood, but it's still definitely making us queasy. If you have the stomach for it, watch our first look at Slednecks above and then get ready for an adrenaline-pumping premiere tonight.
Slednecks premieres Thursday, Oct. 30 at 10 p.m. with an extended 90-minute special on MTV.