Metal Detecting Forum, Metal Detector Reviews, Gold Prospecting and Treasure Hunting Forum � Searching For Other Types of Treasure � Meteorite Hunting, finding and collecting meteorites�... My presumption is that you have found a rock that you think is a meteorite. You want to identify that rock. The intent is that you start here and work your way sequentially through the pages. At the end you will have a better idea whether or not your rock is a meteorite--but there will be more to do.
Meteorite identification Welcome to the home of meteorites!
Meteorite Identification The Meteorite Exchange Inc.
Abstract Have you ever heard someone say that the moon is made of cheese? Even though the craters on the surface of the moon resemble holes in Swiss cheese, we know that this common myth is not true.
Meteorite identification is frustrating because almost all the identification rules have exceptions. The following guidelines may help you determine if you have a meteorite. The following guidelines may help you determine if you have a meteorite.


If you don't fight friendly fraud, your business is suffering a lot of needless revenue loss. Find out how to challenge illegitimate chargebacks and recover revenue that's rightfully yours.
Creating and submitting a chargeback response, sometimes referred to as representment, can be a labor-intensive task. We offer a step-by-step guide for chargeback representment here.
The bulk of that labor-intensive process is just a lot of administrative work—paper-pushing tasks you repeat over and over for each chargeback.
However there are two stages, woven into those repetitive workflows, that require strategizing and intelligent decisions.
If you skip these strategic phases and make the entire process a monotonous activity, you won't be able to successfully fight friendly fraud. You'll invest a lot of resources into a losing cause and kill your ROI.
Which activities require careful thought and consideration?
STRATEGIZING PHASE #1: Figure out what you should and shouldn't fight.
Some chargeback "experts" will tell you to fight everything. After all, if you don't fight, you can't win. However, this strategy is dangerous for two reasons.
First, you could inadvertently challenge a legitimate chargeback. Second, you'll invest time and resources into cases that can't be won, so ROI will be minimal.
Here's how Midigator® suggests merchants fight friendly fraud.
Create strategic fight rules to filter out cases that shouldn't be fought so you're only fighting winnable, ROI-optimized cases of confirmed friendly fraud.
Midigator has automated this phase. The technology knows what should and shouldn't be fought.
If you are managing friendly fraud in-house, you need to create manual processes to evaluate each chargeback and add them to your workflows. Don't skip this important step—your business's reputation and ROI depend on it!
STRATEGIZING PHASE #2: Customize your response.
When you fight friendly fraud, you need an air-tight case.
Cardholders are the bank's customers. When it comes to processing chargeback requests, the old adage, "the customer is always right" reigns. It will take a highly-compelling argument to overturn the chargeback and force the issuer to acknowledge the friendly fraud.
Generic, one-size-fits-all chargeback responses won't be able to do that. They won't win.
Here's where you push pause on the repetitive workflows and insert strategic thinking and intelligent decisions. What will it take to win?
Midigator's technology customizes each chargeback response by dozens of different variables. If you fight friendly fraud in-house, you can use our insights about what works best.
Customize by Processor Preferences: There is a chance your processor could terminate the response and never even send your case to the issuer for review. To ensure the processor accepts your case and advances it to the next stage, you'll need to customize your response to the processor's preferences. Each processor has different expectations, so responses need to adapt. This can include everything from how documents are ordered to the method used for submission.
Customize by Reason Code: Each chargeback is assigned a reason code—a description that helps you understand why the cardholder disputed the transaction. Reason codes also regulate which forms of compelling evidence must accompany your chargeback response. All required evidence should be included, but non-compelling items should be omitted.
Customize by Product Type: Compelling evidence requirements vary by product type. For example, a chargeback response for physical goods will include things like delivery tracking information, and a response for digital goods would contain information about usage and download history.
Customize by Sales Method: Compelling evidence requirements vary by sales method. A chargeback response for a card-present transaction will be different than a response for a card-not-present transaction. Within those different sales environments, disputes should be categorized even more distinctly—PIN transaction, recurring transaction, MO/TO transactions, etc.
Customize by Geographical Location: Regulations vary by geographical location. The issuer's and acquirer's location will impact how a chargeback response is handled. Your response will need to adapt for things like timelines and language requirements.
Unfortunately, you can't create a cookie-cutter template and use it for every chargeback you receive. If you want to win, you have to customize your responses.
Are you Ready to Fight Friendly Fraud?
A tactical approach to revenue recovery achieves the best results possible. However, expecting your in-house team to find time for this added responsibility is asking a lot.
At Midigator, we believe the challenge of running a business should be delivering great products or services, not managing payment risk. That's why we created intuitive technology to automate the entire chargeback response process. You get the best results possible and your in-house team focuses on growing the business.
If you'd like to see how Midigator can help your business fight friendly fraud, sign up for a demo today.
Want Better Chargeback Protection? Do These 7 Things.
Do you want to improve your chargeback protection strategy, but don't know where to begin? Start here: break down the process into these seven manageable steps.
This is the story of how a merchant used Midigator's detailed analytics to prevent subscription billing chargebacks and increase customer lifetime value.
How do you measure chargeback management success? Do you rely solely on chargeback win rates? If so, you are only looking at one small piece of the puzzle. There is so much more to consider.


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i use the incipio feather but now im all for the seidio innocase II with the holster and seidio charger...I love how seidio makes their products to work together all they need to do is make a car holder.
Thanks! Never heard of the incipio feather but will have to take a look.
I bought my cell phone accessories at an ebay store, the name is Monster Accessory, you can find good quality cases holsters, cell phone chargers with decent price.
oh, yes, I bought case for my moto at this store as well. monster accessory, interesting name.
I used to buy my case when ebay, but I found that some online store is cheaper...any suggestions?
I am looking for a case for my BB 9650 and have seen a lot of people recommend this case, others complain its too bulky. Is this case extremely bulky or is it decent size? I am debating between the incipio feather, seidio innocase, and the otterbox defender.
Last edited by jeriel05; 10-06-2010 at 08:18 PM.


text:
\section{Introduction}

Direct detection of gravitational radiation will hopefully soon become a reality, with the operation of the first generation of
 interferometers such as (kilometer-scale, ground-based) LIGO~\cite{LIGOURL} and VIRGO~\cite{VIRGOURL} and (million-kilometer-scale, space-based) LISA~\cite{LISAURL}. Those instruments will allow us to probe gravitational waves produced by astrophysical objects at relatively low red-shift (black hole binaries, neutron star binaries, white dwarf binaries, supernovae, pulsars...)
In addition, gravitational waves (GW) can provide information about particle physics at unexplored high energies.
The weakness of the interaction with matter is a major obstacle for detection of gravitational waves but it also has the virtue that the information they carry about the state of the universe at the moment of their production has been unaltered.
They are precious information on the very mechanism that produced them.
GW can be produced by core collapse of supernovae, first-order phase transitions, vibration of cosmic strings, preheating, dynamics of extra dimensions\ldots

Among those well-motivated but hypothetical cosmological sources of GW, there is at least one that we are convinced exists:   the GW produced during inflation. This signal is expected to be very tiny. Quantum fluctuations in the inflaton field during inflation leaves behind a residue in density perturbations observed in the Cosmic Microwave Background (CMB). They also lead to a background of GW whose properties couple with those of density fluctuations. As the CMB anisotropies are affected by GW, the WMAP constraint on the energy scale of inflation
fixes a bound on the size of the GW signal due to inflation $\Omega_{GW} h^2 \mathrel{\ltap} 10^{-15} -10^{-14}$~\cite{Smith:2005mm}. This is several orders of magnitude below the best sensitivity of the first-generation of interferometers.
However, attempts to detect this relic primordial background are very strongly motivated. This is a main goal of the second generation of space interferometers, in particular, the Big Bang Observer (BBO)~\cite{BBOURL}, the follow-on mission to LISA,  which would become a reality within twenty or thirty years (by comparison, LISA, if funded, should be operational by 2014).

The present work focusses instead on the detectability of GW from first-order phase transitions.
The corresponding relic GW background encodes useful information on these major symmetry-breaking events which took place in the early universe.
In contrast with the inflationary spectrum, the spectrum is not flat, with a characteristic peak related to the temperature at which the phase transition (PT) took place. This  signal can actually be higher by several orders of magnitude than the signal expected from inflation and in some cases can entirely screen it.
One symmetry-breaking event  which for sure took place in the early universe is electroweak (EW) symmetry breaking. What we do not know yet is whether it was a  first order phase transition, in which case it proceeded through  nucleation of bubbles resulting in a large departure from thermal equilibrium. Bubble collision and associated motions in the primordial plasma are sources of gravitational waves.
The characteristic frequency  of the signal is close to the Hubble frequency at the time of the transition $H(T_{EW}) \sim 10^{-14}$~GeV. Once redshifted to today, this corresponds to mHz frequencies,
which is precisely the frequency band that  LISA is sensitive to. It is therefore very exciting that LISA could help providing information on the EW scale, in particular on the nature of
the EWPT.

The GW spectrum resulting from first order PT was computed
 in the early nineties~\cite{Kosowsky:1992rz,Kosowsky:1991ua,Kosowsky:1992vn,Kamionkowski:1993fg} but this topic has not received much subsequent attention, as it was found out that there is no first order EWPT in the Standard Model given the experimental bound on the Higgs mass~\cite{lattice}.
 It was realized ten years after the original calculation of~\cite{Kosowsky:1992rz,Kosowsky:1991ua,Kosowsky:1992vn,Kamionkowski:1993fg} that turbulence in the plasma could be a significant source of GW in addition to bubble collisions~\cite{Kosowsky:2001xp, Dolgov:2002ra}. Subsequently, the authors of~\cite{Apreda:2001us} studied the GW signal due to a first order EWPT in the Minimal Supersymmetric Standard Model (MSSM) and its NMSSM extension. Finally, Nicolis~\cite{Nicolis:2003tg} did a model-independent analysis for the detectability of GW with LISA.

 We believe that it is time to revisit this question for two reasons: The nature of the EWPT will start to be probed experimentally at the LHC.
 Indeed, it depends essentially on the Higgs sector of the theory or any alternative dynamics for EW symmetry breaking.
 In the last few years, new models of EW symmetry breaking have been suggested (little higgs, gauge-higgs unification, composite higgs, higgsless models ...) and the nature (smooth cross-over or first-order) of the EWPT in these new frameworks remains unknown. Second, the technology for gravitational wave detectors has made advances~\cite{Ballantini:2005am} and we think it is timely to  redo a model-independent analysis not only for LISA but also other devices.

LIGO is sensitive to much higher  frequencies (from a few Hz to a few hundreds of Hz) thus it is in principle sensitive to phase transitions  which took place at much earlier epochs. For instance, we will show that if there was a very strong first order PT at temperatures of order $10^7$~GeV, the ultimate stage of LIGO (LIGO-III, correlated) could detect the corresponding peak (as already pointed out in~\cite{Kosowsky:1992rz}).
The second generation of interferometers will be able to say much about the possible existence of early universe first-order phase  transitions. Indeed, BBO will be sensitive to signals from PT which would have taken place in the temperature range $T\sim 100$~GeV-- $10^7$~GeV, even if not necessarily exceptionnally strong.

In this paper, we start with some generalities on stochastic GW backgrounds including the astrophysical background. We also recap what would be the observable redshifted signal we would observe after the GW have propagated forward from the phase transition until today. Section 3 reviews the key formulae used in the theoretical predictions of the GW spectrum due to first-order phase transitions. There is nothing new in this part. However, this formalism had so far only been exploited to study the detectability at LISA of GW due to a first-order electroweak phase transition. In section 4, we apply it to any other phase transitions taking place at higher temperatures and compare them with the sensitivities of not only LISA but also LIGO and BBO.
Predictions can be presented in a model-independent way as a function of two quantities, namely $\alpha$ ($\sim$ latent heat) and $\beta^{-1}$ ($\sim$ duration of the phase transition), which can be computed for any given effective scalar potential describing the transition.
For each temperature, we identify which values of $\alpha$ and $\beta$ lead to an observable signal.
Particle model builders can then test their favourite scalar potential by computing its corresponding values of $\alpha$ and $\beta$ and see whether it can give rise to a detectable GW signal.
We comment on some specific examples of particle physics models.

\section{Astrophysical versus cosmological GW background}

Stochastic backgrounds are random gravitational waves arising from the incoherent superposition of a large number of independent, uncorrelated sources that cannot be resolved individually. They are discussed in terms of their contribution to the universe's energy density, over some frequency band:
\begin{equation}
\Omega_{GW}(f)=\frac{1}{\rho_{\mbox{\tiny crit}}}\frac{d \rho_{GW}}{d \ln f}
\end{equation}
By their very nature, stochastic GW are indistinguishable from the detector noise. Ground-based detectors look for them by coordinated measurements (comparing outputs of multiple detectors to find sources of correlated noise) while LISA can extract the instrumental noise power by combining the signals from its three spacecrafts. For technical aspects related to the detection of a gravitational wave stochastic background, see  Ref.~\cite{Maggiore:1999vm}.

\subsection{Astrophysical foreground}
\label{astro_back}
Searching for GW waves of cosmological origin is an ambitious goal. There is a huge foreground due to astrophysical sources
which in principle makes detection impractical.
Once the signals from every merging neutron star and stellar mass black holes have been identified and substracted,
the primary sources of foreground signals are galactic and extragalactic binaries.
The galactic background produced by binary stars in the Milky Way is many times larger in amplitude than both the extragalactic foreground and LISA's design sensitivity. However, it can be substracted because of its anisotropy, being mostly concentrated in the galactic plane.
Irreducible background comes from extragalactic binary stars and is dominated by emission from white dwarves (WD) pairs. The corresponding GW spectrum was estimated in Ref.~\cite{Farmer:2003pa} where limits are placed on the minimum and maximum expected background signals. Ref.~\cite{Farmer:2003pa} points out that at frequencies $f \mathrel{\ltap} 50$ mHz, there will be too many individual WD--WD sources contributing in each resolution element to be completely resolved and substracted  source by source by missions with plausible lifetimes. However, much of the flux comes from relatively nearby sources, and the WD--WD numbers drop rapidly above 50 mHz. Thus it may be possible for future missions more sensitive than LISA to substract this background at high frequencies~\cite{Farmer:2003pa}.
In our figures, we plot  this background coming from unresolved compact white dwarf binaries assuming that it can be removed at frequencies above 50 mHz.
At higher frequencies, the dominant foreground GW sources are inspiralling neutron star-neutron star, neutron star-black hole and black hole-black hole binaries. These have to be individually identified and substracted. This problem is discussed in~\cite{Cutler:2005qq} and in our BBO  detectability analysis we optimistically assume that this foreground can be substracted.

\subsection{Relic background from cosmological processes}

The GW background due to early universe events is stochastic as the signal comes from the superposition of incoherent sources originating from a huge number of different horizon volumes.
For instance, the size of the horizon at the time of the electroweak phase transition was much
 smaller than today ${(10^{-14} ~\mbox{GeV})}^{-1}$, corresponding to a tiny fraction of degree on the sky today.
Even if we assumed that there were two bubbles per horizon volume
(actually there would typically be several hundreds of them as we will see later),
we would be unable to resolve the signal coming from their collision.
The signal comes from bubble collisions which
took place in many independent universes.

We work in a standard Friedman--Robertson--Walker (FRW) cosmology, $a(t)$ is the cosmological scale factor. At the energy scales considered, we assume a radiation-dominated era.
Gravity waves produced at $T_*$ with a characteristic frequency $f_*$ propagate until today without interacting. Their energy density redshifts as $a^{-4}$ and their frequency as $a^{-1}$. The characteristic frequency we observe today is
\begin{equation}
f=f_* \frac{a_*}{a_0}=f_* \left( \frac{g_{s0}}{g_{s*}}\right)^{1/3}\frac{T_0}{T_*}
\end{equation}
where we used the adiabaticity of the expansion of the universe (meaning that the entropy per comoving volume $S\propto a^3 g_s(T) T^3$ remains constant).
\begin{equation}
g_s(T)= \sum_{i=\textit{\small bosons}}g_i\left(\frac{T_i}{T}\right)^3
+\frac{7}{8}\sum_{i=\textit{\small fermions}}g_i \left(\frac{T_i}{T}\right)^3
\label{gs_definition}
\end{equation}
$g_i$ counts the internal degrees of freedom of the $i$-th particle and the sum is over relativistic species.
Today, $g_s(T_0)\simeq 3.91$ (assuming three neutrino species) and $T_0= 2.725 K=2.348\times 10^{-13}$~GeV. It is convenient to express the frequency in terms of the Hubble frequency at the time of GW production:
\begin{equation}
\label{characteristic_frequency}
f\approx 6 \times 10^{-3} \mbox{mHz}    \left(\frac{g_*}{100}\right)^{1/6} \frac{T_*}{100\mbox{ GeV}} \ \frac{f_*}{H_*}
\end{equation}
The remarkable fact is that for $T\sim 100$~GeV and $f_*/H_* \sim 10^2$, (as expected for weak scale processes as will be explained below), the peak frequency  of the GW spectrum is in the milliHertz, just in the band of LISA.

The fraction of the critical energy density in gravity waves today is
\begin{equation}
\Omega_{GW}=\frac{\rho_{GW}}{\rho_c}= \Omega_{GW*}\left(\frac{a_*}{a_0}\right)^4\left(\frac{H_*}{H_0}\right)^2\simeq 1.67\times 10^{-5} h^{-2}\left(\frac{100}{g_*}\right)^{1/3} {\Omega}_{GW*}
\end{equation}
where we used
\begin{equation}
{\rho}_{GW}={\rho}_{GW*}\left(\frac{a_*}{a_0}\right)^4 \ , \ \ \rho_c=\rho_{c*}\frac{H_0^2}{H_*^2} \  \mbox{and} \ H_0=2.1332\times h\times 10^{-42}~ \mbox{GeV}
\end{equation}
$g_*$ is the number of relativistic degrees of freedom at $T_*$ which enters the definition of the energy density and not the entropy (it is given by Eq.~(\ref{gs_definition})  where the cubic power is replaced by a quartic power). $\Omega_{GW*}$ is the fraction of energy density of the universe at the time of the transition which is in gravitational waves. The peak sensitivity of LISA would correspond
 to detect $\Omega_{GW}h^2  \sim 10^{-11}$. This means that to detect a signal at LISA, we need $\Omega_{GW*}\mathrel{\gtap} 10^{-6}$ while at BBO, we can probe smaller fractions, $\Omega_{GW*}  \sim 10^{-12}-10^{-9}$.

The remaining task is to estimate $f_*$ and $\Omega_*$.
 Theoretical predictions of relic GW backgrounds are subject to large uncertainties which depend on the cosmological mechanism. However, we can get a reasonable estimate of the characteristic frequency, the form of the spectrum and the typical intensity. We will now review the main results in the case of GW produced during first order phase transitions.

\section{GW from first-order phase transitions}

Phase transitions are commonly described by the effective potential of the scalar field (either elementary or composite) responsible for the dynamics.
First-order phase transitions are triggered if there exists a temperature at which a barrier separates two degenerate minima. This happens for instance if there are negative cubic or quartic self couplings for the scalar field.
In this case, phase transitions proceed via nucleation of bubbles of the low-temperature phase within the high-temperature phase.
Bubble nucleation occurs through quantum tunneling and thermal fluctuations.
These bubbles then expand and merge, leaving the universe in the low-temperature phase (commonly the broken-symmetry phase).
As a bubble expands, part of the liberated latent heat raises the plasma temperature while the other part is converted into kinetic energy of the bubble wall and bulk motions of the fluid.
Because of its spherical symmetry, a single expanding bubble produces no gravity waves. Only after bubble collisions destroy the spherical symmetry is gravitational radiation emitted.
High velocities and large energy densities provide the necessary conditions for producing gravitational radiation.
There are two sources of gravitational waves: the actual collision of bubbles and the turbulence in the plasma due to bubble motion.
The resulting spectrum of gravitational waves has been studied in details in~\cite{Kosowsky:1992rz,Kosowsky:1991ua,Kosowsky:1992vn,Kamionkowski:1993fg,Kosowsky:2001xp,Dolgov:2002ra,Apreda:2001us,Nicolis:2003tg}. The turbulence spectrum was recently revisited in Ref.~\cite{Caprini:2006jb}. Re-examination of the bubble collision spectrum is underway~\cite{CDS}.

Remarquably, these predictions only depend on the grossest features of the bubble collisions. Gravitational radiation is insensitive to the internal structure of colliding bubbles, in other words, to the small scale configuration of the scalar field in the colliding region~\cite{Kosowsky:1992rz}.  As confirmed by numerical simulations~\cite{Kosowsky:1991ua}, the {\it enveloppe approximation} works very well. It
 consists in neglecting the dynamics of the collision (overlapping) region. Kinetic energy is supposed to be concentrated in the uncollided (but spherically asymmetric) bubble walls.

Once bubble walls collide, they stir up the plasma at a scale comparable with their radii at the collision time, leading to turbulence which also induces gravitational emission.

\subsection{Key parameters characterizing the GW spectrum}

A crucial parameter for the calculation of the gravitational wave spectrum  is the rate of variation of the bubble nucleation rate, called $\beta$. This quantity fixes the characteristic scale in the problem,
the size of bubbles at the time of the collision, and therefore the characteristic frequency $f_*$.
The duration of the phase transition is given by
$\beta^{-1}$ and the size of bubbles is typically   $R_b \sim v_b \beta^{-1}$ where $v_b$ is the velocity of the bubble wall. The initial size of the bubble at the time of nucleation (of the order of $T^{-1}$) is negligible compared to $\beta^{-1}$ which is of the order of the horizon size.

The second crucial parameter  characterizing the spectrum of gravitational waves is $\alpha=\epsilon / \rho_{rad}$, the ratio of the latent heat liberated at the phase transition ($\epsilon$=latent heat) to the energy density in the high energy phase, commonly being radiation energy density. $\epsilon$ is not necessarily vacuum energy, see for instance~\cite{RS}.
$\alpha$ and $\beta$ are evaluated at the nucleation temperature and determine entirely the GW spectrum.
They can be computed once we know the effective action for nucleating bubbles (``critical bubbles") which can be computed for any scalar potential describing the phase transition. Therefore,
given a scalar potential at finite temperature, $V(\phi,T)$, this is enough to derive the predictions for the GW spectrum.

The rate of bubble nucleation is
\begin{equation}
\Gamma(t)=A(t) e^{-S(t)}
\label{nucleationrate}
\end{equation}
The prefactor $A(t)$ has units of energy to the fourth power,  $A(t)\sim {\cal M}^4$,
 where ${\cal M}\sim T$ is the typical energy scale of the transition and
 $S(t)\approx S_3/T$ is the euclidean action of the critical bubble.
\begin{equation}
S_3=\int 4 \pi r^2 dr \left[ \frac{1}{2}\left(\frac{d\phi_b}{dr}\right)^2 + V(\phi_b,T)\right]
\end{equation}
is the free energy of a critical bubble.
$\phi_b$ is the bubble profile of the critical bubble obtained by solving for the ``bounce'':
\begin{equation}
\label{bounce}
\frac{d^2\phi_b}{dr^2}+\frac{2}{r}\frac{d\phi_b}{dr}-\frac{\partial V}{\partial \phi_b}=0,  \ \ \  \mbox{with} \ \ \ \left. \frac{d\phi_b}{dr}\right|_{r=0}=0 \  \ \mbox{and} \ \ \left. \phi_b\right|_{r=\infty}=0
\end{equation}
Most of the time variation of $\Gamma(t)$ is in $S(t)$, and $\beta$ is defined as:
\begin{equation}
\beta \equiv -\left. \frac{d S}{d t}\right|_{t_*} \approx \left.\frac{1}{\Gamma}\frac{d\Gamma}{dt}\right|_{t_*}
\end{equation}
where $t_*$ is the time when the transition completes. In a neighbourhood of $t_*$, $\Gamma(t)$ grows exponentially with time as $S(t)=S(t_*)-\beta (t-t_*) + ...$.
From the adiabaticity of the expansion of the universe, ${d T}/{dt}=-T H$, where $H$ is the expansion rate of the universe, and we obtain
\begin{equation}
\frac{\beta}{H_*}=T_*\left. \frac{d S}{d T}\right|_{T_*}=T_* \left.\frac{d}{dT} \left(\frac{S_3}{T}\right)\right|_{T_*}
\end{equation}
The temperature of the transition $T_*$ is defined as the temperature at which the probability for nucleating one bubble per horizon volume per horizon time approaches 1. This guarantees that bubbles percolate even if the universe is inflating. This translates into
\begin{equation}
\frac{\Gamma}{H^4} \sim O(1) \ \ \rightarrow S=-4 \ln \frac{{ T_*}}{m_{Pl}}
\label{nucleationcondition}
\end{equation}
$\beta/H $ is dimensionless and mainly depends on the shape of the potential at the time of nucleation. According to (\ref{nucleationcondition}), it depends only logarithmically on the energy scale. For a phase transition at the weak scale $\beta/H\sim 10^2$ and this justifies what we said after
 Eq.~(\ref{characteristic_frequency}) (where $f_*$ stands for $\beta$).
 While the size of the bubble increases by orders of magnitude between nucleation and percolation
 (its initial radius $R\sim \phi/\sqrt{\Delta V}$ at the time of nucleation can be neglected; all what matters is the typical size at the end of the transition
which is given by $R_b \sim v_b \Delta t \sim v_b \beta^{-1}$), $T_*$ (and thus $\alpha$ and $\beta/H$) is essentially unchanged between nucleation and percolation.

Note that the ratio $\beta/H $ also fixes the number of bubbles. The number density of bubbles is roughly $\beta^{-1}\Gamma(t)$ so that the number of bubbles in one horizon volume is $\beta^{-1}  \Gamma/H^3$, which, at the end of the transition is of order $H/\beta$.

The latent heat is the sum of two contributions. The first one is
the difference in free energies between the stable and metastable minima (which vanishes at $T_c$) while the second one comes from the entropy variation $\Delta {s}$ (which is non zero at $T_c$ in a first-order PT). This leads to the following formula for $\epsilon$:
\begin{equation}
\epsilon=-\Delta V - T  \Delta { s}=\left(-\Delta V + T  \partial V/ \partial T \right)_{T_*}
\label{latentheat}
\end{equation}

To conclude, for the analysis of gravity wave emission, the only two relevant quantities are the amount of latent heat injected into the plasma, Eq.~(\ref{latentheat}), and the nucleation rate, Eq.~(\ref{nucleationrate}).  So once  the
bubble action is computed (search for the bounce solution Eq.~(\ref{bounce})), everything is known.
 The fact that the phase transition is described or not by a  fundamental scalar field is irrelevant.

In practise, instead of solving Eq.~(\ref{bounce}), one can use either the thin wall or thick wall limits to approximate the bounce solution. In the regime of large supercooling (which is the one of interest as far as large signals of gravitational waves are concerned), the thick wall approximation is adequate. In addition, if the temperature is decreasing and the ratio $T/T_c$ is getting low ($T_c$ is the critical temperature at which the free energies in the two phases are equal) one can use the 4D euclidean action $S_4$ to evaluate the nucleation rate rather than $S_3/T$.

\subsection{Scaling expectations}

The energy density in gravitational waves coming from bubble collision can be estimated by naive dimensional analysis as follows.
The quadrupole formula for the power of gravitational emission is $ P_{GW}=\frac{G}{5}\langle ( {\stackrel{\ldots}{Q}} _{ij}^{TT})^2\rangle$ where $G$ is the Newton's constant and
$Q _{ij}^{TT}$ is the quadrupole moment of the source which is  $T _{ij}^{TT}$, the transverse traceless piece of the stress tensor.
We can write
\begin{equation}
 {\stackrel{\ldots}{Q}} _{ij}^{TT} \sim \frac{\mbox{mass of system in motion} \times (\mbox{size of system})^2}{(\mbox{time scale of system})^3}\sim \frac{\mbox{kinetic energy}}{\mbox{time scale of system}}
\end{equation}
thus, $P_{GW} \sim G \dot{E}_{kin}^2$.
Let  $\kappa$ be the efficiency factor which quantifies the fraction of the vacuum energy  which goes into kinetic energy of bulk motions of the fluid (as opposed to heating):
\begin{equation}
E_{kin}\sim \kappa \  \alpha \ \rho_{rad} \ (v_b \beta^{-1})^3
\end{equation}
Using $G\sim H_*^2/ \rho_{tot*}$ and $\rho_{tot*}=(1+\alpha)\rho_{rad}$ we get ($d/dt$ leads to a $\beta^2$ factor)
$\rho_{GW*}=E_{GW}/(v_b^3 \beta^{-3})$ where $E_{GW}=P_{GW} \beta^{-1}$. Finally:
\begin{equation}
\Omega_{GW*}=\frac{\rho_{GW*}}{\rho_{tot*}}\sim \left(\frac{H_*}{\beta}\right)^2\kappa^2\frac{\alpha^2}{(1+\alpha)^2}v_b^3
\end{equation}
To get a large signal, we need ${\beta}/{H_*}$ to be small and  $\alpha$ to be large, in other words, the phase transition should last as long as possible and the latent heat should be maximized.
The scaling obtained is very close to what a more rigorous calculation gives for the redshifted value of the energy
density evaluated at the peak frequency~\cite{Kamionkowski:1993fg}:
\begin{equation}
\label{Omegacoll}
\Omega_{\mbox{\tiny coll}} \ h^2 (f_{\mbox{\tiny coll}}) \simeq 1.1 \times 10^{-6} \kappa^2 \left[\frac{H_*}{\beta}\right]^2 \left[\frac{\alpha}{1+\alpha}\right]^2\left[\frac{v_b^3}{0.24+v_b^3}\right]\left[\frac{100}{g_*}\right]^{1/3}
\end{equation}
while the peak frequency is~\cite{Kamionkowski:1993fg}
\begin{equation}
\label{fcoll}
f_{\mbox{\tiny coll}} \simeq 5.2 \times 10^{-3} \mbox{mHz} \left[\frac{\beta}{H_*}\right]\left[\frac{T_*}{100 \mbox{GeV}}\right]\left[\frac{g_*}{100}\right]^{1/6}
\end{equation}
The scaling is slightly  different in the case of GW from turbulence in the plasma (the analysis
of turbulent motions of~\cite{Kosowsky:2001xp} was generalized in~\cite{Dolgov:2002ra, Nicolis:2003tg}):
\begin{equation}
\label{Omegaturb}
\Omega_{\mbox{\tiny turb}} \ h^2 (f_{\mbox{\tiny turb}}) \simeq 1.4 \times 10^{-4} u_s^5v_b^2 \left[\frac{H_*}{\beta}\right]^2 \left[\frac{100}{g_*}\right]^{1/3}
\end{equation}
with~\cite{Dolgov:2002ra, Nicolis:2003tg}
\begin{equation}
\label{fturb}
f_{\mbox{\tiny turb}} \simeq 3.4 \times 10^{-3} \mbox{mHz} \frac{u_s}{v_b}\left[\frac{\beta}{H_*}\right]\left[\frac{T_*}{100 \mbox{GeV}}\right]\left[\frac{g_*}{100}\right]^{1/6}
\end{equation}
The turbulent fluid velocities $u_s$  are smaller than the bubble expansion velocities, unless turbulence is extremely strong. As a result, according to (\ref{fcoll}) and (\ref{fturb}), the peak  for the turbulence spectrum will be shifted to lower frequencies. Note that the peak frequency of the collision signal does not depend on $\alpha$. Because $f_{\mbox{\tiny turb}} \approx f_{\mbox{\tiny coll}}   \times (u_s/v_b)$ and $(u_s/v_b)$ is an increasing function of $\alpha$, as $\alpha$ increases, the collision peak gets hidden by the high-frequency tail of the turbulence signal\footnote{Although the relation $f_{\mbox{\tiny turb}} \approx f_{\mbox{\tiny coll}}   \times (u_s/v_b)$ is likely to be revised in Ref.~\cite{CDS}.} .

The signal from turbulence is more promising than the signal from bubble collision due to the different scaling with $\alpha$. Indeed, the scaling with $\alpha$ of the velocities and the efficiency  factor are :
\begin{equation}
v_b(\alpha)=\frac{1/\sqrt{3} +\sqrt{\alpha^2+2\alpha/3}}{1+\alpha} \  \mbox{~\cite{Steinhardt:1981ct}}  \ \ \  ,  \ \ \ u_s(\alpha)\simeq \sqrt{\frac{\kappa \alpha}{\frac{4}{3}+\kappa \alpha}}  \mbox{~\cite{Nicolis:2003tg}}
\end{equation}
\begin{equation}
\kappa(\alpha)\simeq \frac{1}{1+0.715 \alpha}\left[0.715 \alpha +\frac{4}{27}\sqrt{\frac{3\alpha}{2}}\right] \mbox{~\cite{Kamionkowski:1993fg}}
\end{equation}

The formulae (\ref{Omegacoll})  and (\ref{Omegaturb}) for $\Omega h^2$ show that the amplitude of the signal does not depend on the energy scale of the transition but only on the dimensionless parameters ${\alpha}$ and ${H_* / \beta}$, in other words on  the shape of the scalar potential at the time of nucleation. Very roughly, taking $\beta/H_* \sim S_3(T_*)/T_*\sim {\cal O}(100)$, it is clear that we need $\alpha \sim {\cal O}(1)$ if we want $\Omega h^2 \mathrel{\gtap} 10^{-10}$ (to see something at LISA).
Our experience with possible values of $\alpha$ and $\beta/H_*$ is based on the studies of potentials describing the electroweak phase transition. The values of $\alpha$ and $\beta/ H_*$ are related to the ratio $\phi (T_*)/T_*$, another quantity characterizing the {\it strength} of the phase transition, where $\phi$ is the vacuum expectation value of the Higgs.
For instance, in the Minimal Supersymmetric Standard Model (MSSM), $\alpha$ is typically smaller than 0.1 while $\beta/H_*$ is larger than 1000~\cite{Apreda:2001us}. On the other hand, in the NMSSM, the authors of~\cite{Apreda:2001us} found values of $\alpha \sim {\cal O}(1)$.
Values of $\alpha$ larger than 1 correspond to a phase transition which is so strong that it is at the borderline of not being able to take place because the free energy of a critical bubble is too large: either the barrier separating the two minima is too large (the barrier even exists at zero temperature) or the distance in field space between the two minima of the potential is too big. The same applies if $\beta/H_*$ is smaller than ${\cal O}(100)$.
 This situation is encountered not only in the NMSSM but also in effective theories with large negative quartic couplings~\cite{Grojean:2004xa}, as will be presented in~\cite{Delaunay}. Note that for a given scalar potential, $\alpha$ and $\beta/H_*$ are actually correlated as a large value of $\alpha$ will be associated with a small value of $\beta/H_*$. Indeed, $\alpha$ is proportional to the latent heat, which grows as $\Delta V$, the depth of the potential at the minimum, is getting bigger. On the other hand, $S_3/T$ (and thus $\beta/H_*$) typically scales like $1/\sqrt{\Delta V}$.

 Let us make a few comments  concerning the situation where $\alpha \sim 1$. In usual phase
  transitions,
  this means that the vacuum energy is of the same order as the radiation energy density, therefore inflation starts before bubbles percolate.  However, if Eq.~(\ref{nucleationcondition}) is satisfied, this guarantees that the phase transition can still complete. The number of e-foldings of inflation is
  $\ln (V^{1/4}/T_*)$, which is  typically less than 1. However, if the transition is very slow, i.e. $\beta/H \mathrel{\ltap} 1$, one should take formulae (\ref{Omegacoll}) and (\ref{Omegaturb}) with caution as they are derived neglecting the expansion of the universe, which is not a good approximation if $\beta/H<1$.

  Fig.~\ref{fig:100GeV} shows some GW spectra illustrating the predictions for various temperatures with representative values of $\alpha = 0.4, 1$ and $\beta/ H_*=100, 800, 3000$. Those plots also exhibit
two examples of signals from inflation (and taken from~\cite{Smith:2005mm}) for comparison.
The scale of inflation is constrained by the CMB to be $E_{I}\mathrel{\ltap} 3.4 \times 10^{16 }$~GeV~\cite{Smith:2005mm}. This fixes the largest signal we could expect from inflation as $\Omega_{\mbox{\tiny GW}} h^2\propto E_I^4$. We also include the signal corresponding to $E_{I} = 5 \times 10^{15 }$~GeV which could be observed at BBO.

\begin{figure}[!htb]
\begin{center}
\includegraphics[height=7.cm,width=8.cm]{SpectT10E2.eps}
\includegraphics[height=7.cm,width=8.cm]{SpectT10E3.eps}
\includegraphics[height=7.cm,width=8.cm]{SpectT10E4.eps}
\includegraphics[height=7.cm,width=8.cm]{SpectT10E7.eps}
\caption{Spectrum of gravitational waves expected from a first order phase transition (solid blue line) for four temperatures and for some choices of ($\alpha, \beta/H$) values. The dashed red lines are the (approximate) predicted sensitivities of LISA, BBO, LIGO-III. The horizontal dashed green lines are the gravitational spectra expected from inflation, for two scales of inflation, for comparison. The black dashed curve is the estimate for the irreducible foreground due to white dwarf binaries (from~\cite{Farmer:2003pa}). At large $\alpha$, only the peak from turbulence can be seen as well as a change of slope (shown as a circled cross) corresponding to the high frequency tail of the bubble collision spectrum. For low $\alpha$, it is possible to see the collision peak as well.}
\label{fig:100GeV}
\end{center}
\end{figure}

\section{Scanning the ($\alpha$, $\beta/H_*$) plane}
In our analysis below, we will use the formulae of the previous section as well as the fact that the spectrum $\Omega_{\textrm{\tiny coll}} h^2 $ is expected to increase as $f^{2.8}$ while at high frequencies it drops off as $f^{-1.8}$ and that $\Omega_{\textrm{\tiny turb}}  h^2$ increases as $f^{2}$ while at high frequencies it drops off as $f^{-7/2}$. This is already all summarized in the letter~\cite{Nicolis:2003tg}. However,  Ref.~\cite{Nicolis:2003tg} focuses on the detectability at LISA of GW from a $T=100$~GeV phase transition. We are now using this formalism to look in more details at the detectability of GW coming from any other 1st order phase transitions at future interferometers.
We repeat that  we are working at the level  of an-order-of-magnitude estimate.
Magnetohydrodynamical effects could make the slope of the turbulence high frequency tail smaller~\cite{Nicolis:2003tg} and in any case, for a more precise analysis, the calculation of the power spectrum should be revisited first.
We compare the GW spectra resulting from PT occurring at temperatures in the range $[100~\mbox{GeV}, 100~\mbox{PeV}]$ with the sensitivities of LISA, BBO and LIGO correlated third generation (and taken from
\cite{Buonanno:2004tp}).
The BBO sensitivity is approximate and may change in the final design. We are actually using the sensitivity of BBO Corr, its correlated extension, which correlates two detectors, namely two LISA-like constellations (each LISA-like constellation orbits around the Sun at 1 AU and consists in three spacecrafts in a triangular
configuration) that will allow to do correlations to measure the
stochastic background. As discussed in Section~\ref{astro_back}, we take into account as well the irreducible background due to extragalactic white dwarf (WD) binaries.

 \begin{figure}[!htb]
\begin{center}
\includegraphics[height=7.cm]{Different_Shapes_Spectra_ai.eps}
\caption{Different configurations of the signal versus the instrument sensitivity to show the qualitative dependence on parameters. The upper blue region is where the turbulence peak is observable while the lower red one is the region where either the collision peak or the point of slope change is  visible.
Precise locations of these different regions depend on the experiment and the temperature of the transition as illustrated in Figs.~\ref{fig:LISAcontours}, \ref{fig:BBO} and~\ref{fig:LIGOcontours}.}
\label{fig:regions}
\end{center}
\end{figure}

For each temperature, we are making a full scan of the ($\alpha$, $\beta/H_*$) parameter space and determine the regions where at least one of the peaks is observable.
According to Eq.~(\ref{Omegacoll}, \ref{fcoll},\ref{Omegaturb},\ref{fturb}), various situations can arise:

\begin{itemize}
\item For relatively low $\alpha$, the turbulence and collision peaks are well separated and can be observed. This is the ideal situation as the observability of these two peaks would be a smoking gun for the phase transition origin of these GW. The ratio of the two peak frequencies is a predicted function of $\alpha$. In somes cases, the turbulence peak is at too low frequency to be observed by LISA or BBO but the minimum separating the two peaks is visible.

\item At larger $\alpha$ ($\mathrel{\gtap}$ 0.64), the collision peak is hidden by the high frequency tail of the turbulence peak. However, there is a characteristic change of slope in the high frequency tail. Depending on the temperature of the transition, this change of slope can be observed or not.
\end{itemize}

\begin{figure}[!htb]
\begin{center}
\includegraphics[height=4.9cm,width=8.cm]{LisaT50.eps}
\includegraphics[height=4.9cm,width=8.cm]{LisaT10E2.eps}
\includegraphics[height=4.9cm,width=8.cm]{LisaT500.eps}
\includegraphics[height=4.9cm,width=8.cm]{LisaT10E3.eps}
\includegraphics[height=4.9cm,width=8.cm]{LisaT10E4.eps}
\includegraphics[height=4.9cm,width=8.cm]{LisaT10E5.eps}
\includegraphics[height=4.9cm,width=8.cm]{LisaT10E6.eps}
\caption{Contours delimiting the region in the ($\alpha$, $\beta/H$) plane for which there is an observable peak at LISA. The upper blue region is for the turbulence peak while the lower red one is the region where either the collision peak or the point of slope change is  visible. Left of the vertical green line, the collision peak is visible.}
\label{fig:LISAcontours}
\end{center}
\end{figure}

Our contour plots show the region where the turbulence peak is observable and the region where either the collision peak or the slope change is visible, at LISA (Fig.~\ref{fig:LISAcontours}), BBO (Fig.~\ref{fig:BBO}) and LIGO (Fig.~\ref{fig:LIGOcontours}). The vertical line separates the low $\alpha$ region where the two peaks are well separated  from the large $\alpha$ region where only the change of slope is visible. The lower horizontal bound is due to the fact that we cut the sensitivity of both LISA and BBO at $10^{-4}$ Hz. Because of this frequency limit in the sensitivity, we cannot probe phase transitions below a $\sim$ GeV and thus the QCD phase transition.  In the BBO plots, we show the very important effect of the WD foreground on the detectability at BBO.

 Note that we could have also made contours corresponding to cases where none of the peaks are observable but the high or low frequency tails can still be detected. This will clearly enlarge the detectability region and this is work in progress.

\begin{figure}[!htb]
\begin{center}
\includegraphics[height=4.9cm,width=8.cm]{BBOT50.eps}
\includegraphics[height=4.9cm,width=8.cm]{BBOT10E2.eps}
\includegraphics[height=4.9cm,width=8.cm]{BBOT500.eps}
\includegraphics[height=4.9cm,width=8.cm]{BBOT10E3.eps}
\includegraphics[height=4.9cm,width=8.cm]{BBOT10E4.eps}
\includegraphics[height=4.9cm,width=8.cm]{BBOT10E5.eps}
\includegraphics[height=4.9cm,width=5.33cm]{BBOT10E6.eps}
\includegraphics[height=4.9cm,width=5.33cm]{BBOT10E7.eps}
\includegraphics[height=4.9cm,width=5.33cm]{BBOT10E8.eps}
\caption{Same as Fig.~\ref{fig:LISAcontours} but for BBO. The effect of including the constraint from the irreducible WD foreground is displayed and limits the observable regions from the uncolored ones to the ones in plain colors. As the temperature increases, the peaks are shifted to higher frequencies, thus the effect of the WD foreground becomes less significant.}
\label{fig:BBO}
\end{center}
\end{figure}
\begin{figure}[!htb]
\begin{center}
\includegraphics[height=5.cm,width=8.1cm]{LigoT10E7.eps}
\includegraphics[height=5.cm,width=8.1cm]{LigoT10E8.eps}
\caption{Same as Fig.~\ref{fig:LISAcontours} but for LIGO-III.}
\label{fig:LIGOcontours}
\end{center}
\end{figure}
\begin{figure}[!htb]
\begin{center}
\includegraphics[width=12cm]{InflationBBO_final.eps}
\caption{Below each line (each one associated with the temperature of the phase transition), the gravitational wave signal at BBO from 1st order phase transitions entirely masks the signal expected from inflation. This plot strongly depends on the scale of inflation, which was chosen here to be $E_I= 3.4 \times 10^{16}$~GeV.}
\label{screen}
\end{center}
\end{figure}

\subsection{ T=100 GeV}

LISA will be able to detect the peak of GW from a 100~GeV first order PT only if it is extremely strong ($\alpha \mathrel{\gtap} 0.5$ or $\beta/H \mathrel{\ltap} 1000$).
The Higgs potential of the MSSM does not satisfy this requirement but it can in the NMSSN~\cite{Apreda:2001us}. Higgs potentials with negative quartic couplings can also trigger strong EWPT as was shown in~\cite{Grojean:2004xa}. The corresponding prospects for GW detection will be presented in details elsewhere~\cite{Delaunay}. There are also exciting large signals expected from the high temperature behaviour of a warped extra dimension~\cite{RS}.
If $T$ is $\sim 500$~GeV rather than 100~GeV, the GW peak will coincide with LISA's best sensitivity frequency and a larger region will be detectable.
The prospects for detection of GW from the 100~GeV EWPT are very good at BBO. At these low frequencies, the WD foreground is lower.  For instance, the turbulence peak for $\alpha \mathrel{\gtap} 0.3$,
${\beta}/{H}\sim 200$, is above the WD foreground and can be seen by BBO.
Note also that at $T=500$~GeV, values of $\beta/H$ as large as $10^4$--$10^5$ can  be probed.

\subsection{T=1 TeV}

It is quite exciting that a 1 TeV PT with $\alpha \mathrel{\gtap} 0.4$, ${\beta}/{H} \sim 200$ can be seen by LISA.
Recent radical proposals to address the hierarchy problem predict rich new phenomena at the TeV scale. For instance, new dimensions at a TeV could give rise to observable signals at LISA~\cite{RS}.
There was also a recent study of the high temperature behavious of Little Higgs Theories where it was shown that EW symmetry was restored precisely at a temperature of order $\sim$ 1 TeV~\cite{Espinosa:2004pn}. This transition appeared to be first order. A more detailed analysis would be required to determine whether this PT could be strong enough to lead to an observable spectrum of GW at LISA. Unfortunately, this takes place in the regime where the effective theory ceases to be under control. This is  nevertheless an interesting prospect.

If ${\beta}/{H} \mathrel{\gtap} 100$, the turbulence peak is above the  WD foreground for $\alpha \mathrel{\gtap} 0.2$,  and thus can be seen by BBO. In addition, BBO can see the high frequency tail of the collision peak which covers good part of, if not entirely,  the inflation signal.

\subsection{T=10 TeV}
At these temperatures, the peak cannot be probed by LISA, unless ${\beta}/{H} < 10^2$. On the other hand, LISA can still probe the low frequency tail of these spectra and is therefore a compelling tool to probe scales that LHC will not be able to reach.
As the temperature increases, the peaks are shifted to higher frequencies, thus the effect of the WD foreground becomes less significant and quite weak first order phase transitions can be probed.
And the high frequency tail of the collision peak can entirely screen the inflation signal, depending on the scale of inflation (see Fig.~\ref{screen}).
If ${\beta}/{H}\sim 1000$, it is possible to see both the turbulence and the collision peaks for $0.1 \mathrel{\ltap} \alpha \mathrel{\ltap} 0.64$ and assuming that the inflationary scale is sufficiently low. For ${\beta}/{H} \sim 200$, the collision peak can be seen for $\alpha $ as low as $\sim $0.05 if  the inflationary signal is below the BBO sensitivity.

\subsection{T=100 TeV}

If ${\beta}/{H}\sim 200$ and $\alpha \mathrel{\gtap} 0.2$ the inflation signal is for sure entirely covered.  If the inflation scale is below $\sim 5 \times 10^{15}$~GeV,  $\alpha $ as low as 0.05 could be detected at BBO.
Two peaks can be seen if $0.1 \mathrel{\ltap}  \alpha \mathrel{\ltap} 0.64$  and ${\beta}/{H}  \sim$ 200. At larger ${\beta}/{H}$ only the turbulence peak will be seen.

\subsection{T=$10^7$ GeV}

This is a particularly interesting case as the same signal could be observed by both BBO and Ligo-III. Specifically, a phase transition with $\alpha=0.8$ and ${\beta}/{H}  \sim$ 200 would give a turbulence peak observable by Ligo-III while the low frequency tail would be observable by BBO. In this example, the inflation signal would be hidden except in a very narrow frequency range between 50 mHz and  80 mHz. \\

Interesting signatures end at this energy scale. Phase transitions at T$\mathrel{\gtap} 10^8$~GeV cannot be probed by any of the planned interferometers.

\section{Conclusion}
We have shown that the GW background from early universe phase transitions may become relevant for a second generation detector such as the Big Bang Observatory (BBO) which is so far motivated to detect the GW background produced during inflation.
LISA, LIGO and BBO will be able to probe part of the history of the universe in the temperature range 100~GeV--$10^7$~GeV. The GW signal coming from particle physics phase transitions is directly related to the scalar potential describing the evolution of the order parameter. Observation or non-observation of GW will allow to put constraints on the parameters of these potentials.
The measurement of the GW spectrum (peak frequency and intensity) can discriminate among different models (once combined with experimental measurement at colliders, for instance, once knowing the higgs mass) and put constraints on the model parameters. For example, at LHC, we will be able to measure the Higgs mass but not the quartic or cubic self coupling of the Higgs.  Only a linear collider can provide this information, which timescale could be beyond LISA. LISA could start constraining model parameters before a linear collider. In addition, LISA is sensitive to the 10 TeV scale which is beyond the reach of the near future collider experiments.

The gravitational wave signal from phase transitions at around 10--100~TeV temperatures could entirely screen the signal from inflation, which detection is one of the main motivations for building BBO.

We emphasize that our quantitative analysis can only be indicative given the uncertainties both at the experimental and theoretical level. The sensitivities of LISA, LIGO-III and BBO will certainly change during the next years. On the theoretical side, we use the estimate of the GW power spectrum of~\cite{Kosowsky:1992rz,Kosowsky:1991ua,Kosowsky:1992vn,Kamionkowski:1993fg,Kosowsky:2001xp, Dolgov:2002ra,Nicolis:2003tg} which is enough for the point of this paper.
However, it certainly deserves improvement. We do not venture into this aspect in this work and just encourage that this question be re-examinated given the exciting experimental  prospects for GW detection from phase transitions we demonstrated in this analysis.

\section*{Note added}

As this work was being completed, Ref.~\cite{Caprini:2006jb} appeared where they re-examined the calculation of the gravitational wave background from turbulence. They disagree with and correct the dispersion relation used for gravitational waves in~\cite{Kosowsky:2001xp,Dolgov:2002ra,Nicolis:2003tg}. This leads, in particular, to a different prediction for the peak frequency as well as a different spectral dependence.  Re-examination of the bubble collision spectrum is underway~\cite{CDS}. These new results can marginally affect the detectability regions of Figs.~\ref{fig:LISAcontours}, \ref{fig:BBO} and~\ref{fig:LIGOcontours} but the overall conclusions will remain the same.

\section*{Acknowledgments}

We are indebted to Alessandra Buonanno for very useful discussions. We also thank A.~Nicolis for a clarification on his work, M. Maggiore for pointing out some reference as well as C.~Caprini and R.~Durrer for discussions and finally James Wells for stimulating conversations at the early stage of this project.

redpajama_set_name: RedPajamaArXiv


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A black border set in the print dialog will not be printed. This problem exists with version 19.1.0.
Sorry for the frustration. This is a known issue and our engineers are looking into it.
This reply was created from a merged topic originally titled Photoshop print border not working after 19.1.1 (and still not at 19.1.2).
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text:
Q: How can i use on blur function in AMP? I am using amp-script and i want to use on blur function in amp. when i use this in my file .. it is giving error onblur is not a function ..
Basically I want to do this when I touch on my div tag. I want to focus out from my input text.
1 - Html File
<amp-script layout="container">
  <input type="text" class="demo-input">
  <button class="demo-button">Try me</button>

1

2

3

</amp>

2- js File
    const touchstart = document.querySelector("touch");
  touchstart.addEventListener("touchstart", () => {
    document.querySelector(".demo-input").blur();
  });

Please give me some solution
thanks in advance

redpajama_set_name: RedPajamaStackExchange


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Kaiser Permanente hospital signage
Corporate logos and building signage are the proud public faces of an organization.
In early 2015 I got a call from the project manager handling the rebuild of the Kaiser Permanente Redwood City Medical Center. He asked if Heritage Resources might be interested in the old signage from the sides of the 1968 building designed by Portland, Ore., architects Wolff and Zimmer.
My answer was immediate. "Are you kidding? Of course!"
A year and a half later I finally drove my van over and picked them up. Our archive does not have a lot of objects — most of what we have are photographs and documents — and these artifacts were glorious physical treasures from an important medical facility.
Old Redwood City Medical Center showing palimpsest of former signage — "KAISER FOUNDATION HOSPITAL," 2014
The lettering is distinctive and was common to the whole suite of Henry J. Kaiser's many international industries from the 1940s through the late 1960s — steel, aluminum, cement, engineering, and even the proud lone survivor, the Kaiser Permanente Health Plan. The huge word KAISER in a version of this lettering (note the slightly different "K") graces the side of Oakland's iconic Kaiser Center, which was built in 1960.
But what exactly is this lettering? It's not full-blooded anything but was produced specifically for Kaiser. We don't know if it was done in-house or by an outside design firm. California typographic historian Alastair Johnston thought it was "… probably influenced by Aldo Novarese, who designed Microgramma type." Noted American design author Steven Heller chimed in: "… kind of looks like a [reworked] version of Eurostyle, the O is almost square or like an outline of a TV set. Novarese also designed Eurostile, it's the same family of square-based gothics. [Kaiser] … overemphasized the italic."
Digitally assembled signage recreation from individual letter photos that reads "Kaiser Foundation Hospital"
Regardless of typographic pedigree, these 15-inch tall letters are powerful historic artifacts. They were handcrafted from heavy gauge sheet steel, enameled the equivalent of our brand's Pantone 307 blue. They held up very well over 46 years of exterior use.
Corporate logos and building signage are the proud public faces of an organization. These physical veterans extracted from Redwood City have now been retired to fulfill a new role in sharing our history.
Kaiser Foundation Health Plan logo, 1959
Kaiser Foundation Health Plan logo, circa 1970 (changed 1984)
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redpajama_set_name: RedPajamaCommonCrawl


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Hester is an 1883 novel written by Margaret Oliphant. It examines the cycle of history through the lives of the Vernon family. The book was published in three separate volumes corresponding to three parts of the story. The novel was adapted (and the story reoriented) by Kate Clanchy and Zena Forster for broadcast by BBC Radio 4 in 2013, showing Hester as a determined organizer successful for years but ultimately defeated by the male world of Victorian business.

Plot

Part 1
The Vernon's Banking House is a thriving bank in England. After Mr. Rule, a clerk in the bank, hears rumors about a potential collapse of the bank, he seeks out bank owner John Vernon, but finds that Vernon has disappeared. Mr. Vernon's wife has no information about his disappearance or matters of the bank. However, Catherine, a part-owner of the bank, uses her fortune to stop a run on the bank.

Decades later, Mrs. Vernon and her 14-year-old daughter Hester move back to Redborough. When Hester meets Catherine, she forms an unfavorable impression, but she makes friends with Edward, who is Catherine's confidante and protege.

Five years later, Hester befriends the elderly Morgans, suffers through family dinners and rebuffs a marriage proposal from Harry, another of Catherine's proteges.

Part 2
The Morgans' grandson Roland, briefly introduced in Part I, is developed as a love interest for Hester. The Morgans express their concern about his character in part due to his job as a speculator.

Ellen starts hosting tea dances, which allow the youths to mingle unsupervised and Hester to 'come out' in society. Mrs. John Vernon is excited to help her daughter Hester come out. Additionally, Mrs. Vernon's pearls, which she gives to Hester, provide a point of contention.

Roland's sister Emma then comes to stay with the Morgans. She tries to get herself invited to the dances so that she may also 'come out' and marry. Meanwhile, Edward makes his interest in Hester known and his discontent with Catherine grows.

Hester nearly finds out about her father at one of Catherine's parties.

Part 3
Hester's love life is revisited and marriage is discussed, while Roland talks business with Edward and Harry. Harry is opposed to speculating with the bank's money, but Edward seems enthusiastic.

Edward's betrayal hurts Catherine, as well as harming the bank's business. Edward runs away and marries Emma.

Afterwards, Catherine and Hester work together to retain the bank's status and stability.

The name Hester is a Persian name. It means "Star".

Characters
 Catherine Vernon: The matriarch of Redborough and the Vernon family. Catherine saved the Vernon family bank many years before with her fortune and willpower.
 Edward Vernon: A cousin of Catherine Vernon's and one of the partners in the bank. Catherine's favorite.
 Harry Vernon: Another cousin of Catherine's and the other partner in the bank. Viewed as dull by other characters, he is practical and business-minded.
 Ellen Vernon: Harry's sister. She lives in the White House with her brother and marries Algernon Merridew.
 Hester Vernon: The titular character of the novel and a cousin of Catherine. The daughter of the man who ruined the bank, she is one of Catherine's poorer relatives.
 Mrs. John Vernon: Hester's mother and the widow of John Vernon. She arrives at the Henronry impoverished.
 John Vernon: Catherine Vernon's cousin. He caused the run on the bank that led to Catherine Vernon's intervention.
 Mildmay Vernon: A gossipy, spiteful cousin of Catherine. He spends his days belittling Catherine and the Vernon-Ridgeway sisters.
 Miss Vernon-Ridgeways: Two spiteful cousins of Catherine's. They have a less negative view of Catherine than Mr. Mildmay, but they criticize her every move regardless. Typical Victorian-era spinsters.
 Mrs. Reginald Vernon: A widowed cousin of Catherine. She lives on the opposite side of Hester, who spends her days educating Mrs. Reginald's three children.
 Captain Morgan: Catherine's uncle, a retired and venerable sea captain. Grandfather to Roland and Emma Ashton.
 Mrs. Morgan: Aunt of Catherine, wife to Captain Morgan, and grandmother to Roland and Emma Ashton.
 Mr. Rule: Semi-retired clerk of the Vernon bank. One of the few characters not related to Catherine Vernon, he helps the Vernon cousins oversee the day-to-day operations of the bank.
 Roland Ashton: Grandson of the Morgans and a stockbroker. Love interest of Hester's.
 Emma Ashton: Granddaughter of the Morgans, with no occupation. She spends her time at the Henronry looking for an eligible bachelor and sets her eyes on Reginald Merridew.
 Algernon Merridew: A clerk at the Vernon bank. He eventually marries Ellen Vernon. Brother of Reginald Merridew.
 Reginald Merridew The younger brother of Algernon Merridew who works in his father's office. He hopes to marry Emma Ashton.

Further reading

References

External links

Victorian novels
1883 British novels

redpajama_set_name: RedPajamaWikipedia


The forays by the WAAPA Performance Making course's graduating class to the Blue Room Theatre for the double-head "Tilt" programme have become an annual highlight.
That's in part for their own sake – eight short pieces over two seasons with the freedom, expressiveness and self-indulgence (not always a bad thing) that, maybe, will never come again, will always reveal some delights.
It's also a window into the future; what these young theatre-makers are interested in, and how they deliver it to audiences, will more than likely be the matter and method of the independent stage in time to come.
There's a very direct pay-off from that – along with a trap for young players. Some of the best (or, more correctly, more substantial) "Tilt" bits have quickly gone on to become fully-fledged productions at the Blue Room, albeit with mixed results.
The problem, the challenge anyway, is converting a 25-30 minute piece into the hour-or-so that alternative theatres, fringe festivals and the like trade in.
Sometimes these short shows are exposed as skits when a longer format calls for more character development and a more sustained narrative. Sometimes they leap that tall building with a single bound.
Last year's showstopper, The View From the Penthouse, is a case in point. It's slotted to return, with a longer running time and a shorter title – just Penthouse – at the end of next month in the Blue Room.
From what I saw last year, I'd advise you to crawl over broken glass to see it – but that trap is baited and waiting.
So, to this year's Tilts.
Courtney Henri and Jordan Valenti's play-within-a-play about street performers, a flying whale and surface tension, Fluke, was deftly managed and sweet, without quite nailing its allegory or compelling our attention.
Evelyn Snook, in her Work in Progress, certainly does. A small, sad portrait of a girl battling depression and inertia ("Sometimes it's okay if the only thing you do today is breathe"), it's beautifully written and winningly performed.
The evening's closer, and its most striking performance, was Girl & Thing, a kinetic, sometimes frightening dance piece devised and performed by the busy Courtney Henri and Marshall Stay, who also delivered an impressive video and sound design (with Ash Lazenby). Henri is an extraordinary sight, diminutive, a shock of hair and a frenzy of movement, sometimes defying your senses to keep up with her. I'm tempted to wonder whether Henri and Stay always knew what they were saying in Girl & Thing, but if the language they used to say it was sometimes incomprehensible, the effect was certainly mesmerising.
I'm cheating. The best was first, not last, but I've saved it anyway.
Cookies and Cream (or, as its writer Zachary Sheridan and director Amelia Burke would have it, "however the diddly is done") is everything you could want in forty minutes of alt-theatre. Smart, screamingly funny, did-she-really-SAY-that-ish, snappy, crackly and poppy, it's the antidote to whatever ails you.
And, among the terrific cast of Sheridan, Christopher Moro and Tamara Creasey, a star is born in Elise Wilson – anyone who loves the work of The Last Great Hunt's fabulous Arielle Gray is gong to really love this gal.
Cookies and Cream will be back. You can bet on it.
The second programme (which ends this Saturday 8 September) may not have a firecracker like Cookies and Cream, but it's textually more substantial than the first.
The opener, The Painfully True Story of the Show we Couldn't Make, devised and performed by Noemie Huttner-Koros, Karina White and Snook is a backstage procedural about, as the title suggests, the difficulty – and even the validity – of nice, young, white folk making theatre about people without their privileges. It's a good and worthy idea, blunted by an overabundance of long, meaningful looks and some lengthy, problematic recorded segments that had plenty of verbatim but not enough theatre.
Dad is Isaac Powell, Jarryd Prain and Stay's emotional paean to those strange creatures that fathered us. It's, perhaps, a little repetitive, but it sneaks up on you, building bit by bit to a touching, insightful kind of father-son catharsis – and a pillow fight. It's performed with energy and commitment and should both extend and tighten up nicely if it goes around again some time. The pillows are inspired.
Clare Testoni has made quite a splash over recent times with her combination of shadow puppetry and fairy tale-telling, and it's a lode that Chloe-Jean Vincent, co-creator Madeleine McKeown and co-writer Valenti mine effectively in Where the Woodsman Cannot Find You. Working with the fairytales The Big Bad Wolf, Little Red Riding Hood and Jack and the Beanstalk, Vincent and fellow performers Henri and Stay deliver a multi-media take on the stories, and the head of the girl imagining them, that is tightly-drawn, funny and sometimes genuinely scary.
Who knew the story of Ada – Augusta Ada King, Countess of Lovelace – the only legitimate child of Lord Byron and, some claim, the writer of the first computer programme? Wikipedia, naturally, the writer and director Huttner-Koros, clearly, and now all of us who saw her smartly staged and delightfully composed little bioplay about this extraordinary (Queen) Victorian woman. Played with corseted good grace by McKeown, well supported by Snook, Burke, Creasey and White, Ada is another Tilt that could easily re-emerge as a fully realised-piece in a Spiegeltent near you sometime soon.
Although Programe One's season has finished, you can catch the "TILT" Programme Two at the Blue Room Theatre, 5-8 September.
Pictured top: The terrific cast of 'Cookies and Cream', L-R, Zachary Sheridan, Tamara Creasey, Christopher Moro and Elise Wilson. Photo: Stephen Heath Photography.
This review appears on "From the Turnstiles" and is published on Seesaw with the kind permission of David Zampatti.
'Ada' is another Tilt that could easily re-emerge as a fully realised-piece in a Spiegeltent near you sometime soon. Photo: Stephen Heath Photography.


Jojoba Oil has anti-inflammatory effect, moisturizes the skin. In condition of regular use it makes the skin smooth and shiny. Currant Extract has anti-inflammatory effects, fights age spots, vitaminizes and tones the skin, neutralizes free radicals.
Ingredients: Sodium bicarbonate, Citric Acid, Simmondsia Chinensis oil (jojoba oil), Ribes Nigrum extract (currant extract), Aqua, Perfume, CI 60730.


New job, new life. You were super excited about meeting your fellow workmates, getting that promotion you had been dreaming of for so long, moving up a little in the pay scale, and making your professional goals come true. You arrive to your new office, turn on your computer, open the web browser and —as if it was a genetically conditioned instinct— you log on to Facebook, but only to find out that the page has been blocked. You try with a different browser. The same result. It is the same for Youtube, Spotify, Reddit...the only concern of your workplace is work and that's it. It is a bitter pill to swallow and so begins the day that was supposed to be one of the best in your life.
Anxiety and even anger are some of the symptoms that accompany social media withdrawal. Though it might sound crazy, life in many ways is increasingly resembling science fiction dystopias where the virtual world engulfs all sense of reality.
Yes, it can be annoying to be deprived of your right to use social media at work, but you probably underestimate how liberating it can be to not access Facebook, lose your cell phone, or have no Wi-Fi. When we get away from the virtual word, our minds expand and we are able to spot the little things we might take for granted. Even though you might think you're hiding under a rock, far from it, you're expanding your horizons.
That notice at the restaurant that says: "We have no Wi-Fi, talk to each other" is really annoying, isn't it? Yet, it is becoming increasingly common. Some people are trying to rectify that disrespectful practice that is posting on Facebook while somebody is trying to talk to you. Without social media, you have no choice but to talk to the person you have in front of you, whether you're getting bored in a party or in a work meeting.
With the help of social media we can learn almost anything we want about a person. It's scary. You just have to Google a name or search it on Facebook to open the doors to their privacy. Network security measures are really fragile, and if a person doesn't know how to set them up correctly, anyone can get access to their photos, their past, their comments, and their stories. The absence of social media forces you to interact, make questions, get surprised, and make your own conclusions about who that person really is.
Many companies ban any access to social media for the sake of one thing: productivity. Even if you are at home, it can be good for you to give this a chance. Reading is a habit that many of us have lost because of the Internet, but if we take a book, determined to stop checking notifications or updates, well definitely be able to read a big chunk of it without getting distracted.
Similarly to books, watching a movie became a multimedia experience, but some cinematographic works really need all your attention, and without Facebook, it is easier to understand what you see and what is happening. Likewise, to stop taking photos just to show them off can make you appreciate more those live performances in front of you. Needless to say that taking photographs or filming is useless, as the event has gone through a series of filters that will never be faithful to what you really saw.
Social media filters all of your interests to keep you logged. Their algorithms are designed to give you whatever you want. Once you log out, you have to find information by yourself again. It may sound archaic, but if you try to do this one day, you'll realize you're living in a bubble of complacency that lacks a complete picture of anything.
Facebook is in constant change; whatever is trendy at 10 a.m. becomes irrelevant 12 hours later. However, those who live attached to social media pride on their knowledge about these topics. When you give a chance to forget about Facebook for a while, you realize that you don't care about other people's live and how many likes they get or how many scandals they are mixed up in. It's none of your business. You can enjoy time with your loved ones instead.
You are already able to do all the things listed above with or without Facebook. You just have to remember that your life is much more than posts in a social network. Come back to the real world and rediscover those things you used to enjoy but forgot about because of some comments and likes.


Rafter tables are commonly imprinted on the steel square (carpenter square, rafter square, framing square). I've revised it a bit to include angles of the side cuts for hip and valley and the jack rafters.
For info on how to use these tables see Rafter Tables on the Framing Square.
The angles shown are to be used with the popular compound miter or cutoff saws.
The common rafter is one of a series of lineal structures extending from the fascia of the overhang to the top of an exterior wall to the ridge board of a roof. The angle given for a common rafter is called the plumb cut, since the ends are vertical or plumb. The plumb cut on a common rafter is at the ridge, the bird's mouth on the wall and at the fascia.
The hip rafter is the structural board which forms the hip at an outside corner of the roof and is installed between 2 common rafters at the ridge. The valley rafter is the structural board which forms the valley at an inside corner of the roof. Both the hip and valley rafters form a 45 degree angle, compounded with the slope of the roof. The angle or plumb cut for a hip or valley rafter, given in our table, is taken from the rafter square based on the slope of the roof and diagonal. If the common rafter has a slope of 5" in 12", the hip or valley rafter has a slope of 5" in 17". 17" is the diagonal of a 12" square. The compound angle for the hip or valley rafter is the plumb cut, given in the table, and the degree on each side of this cut, on both ends, as In the table.
There are two types of jack rafters: the hip jack and the valley jack. The hip jack is a short rafter that spans from the wall plate to a hip rafter. The valley jack goes from a valley rafter to the roof ridge. Each jack rafter has the same side cut and plumb cut on the hip or valley rafter and the same angle as the common rafter at the ridge or fascia. The side cut is the angle given in the table, the plumb cut is the same angle as in the table for the hip or valley rafter.


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Articles tagged: Pablo Sandoval
Bruce Bochy will not rule out using Pablo Sandoval to pitch again
Pablo Sandoval was impressive enough as a pitcher on Saturday that San Francisco Giants manager Bruce Bochy will consider doing it again if he has to.
Sandoval touched 88 MPH on the gun and mixed in
Pablo Sandoval 'almost cried' after ending season with walk-off home run
It's been a strange and emotional season for Pablo Sandoval, so it's only fitting that his year ended in a strange and emotional way.
Sandoval ended 2017 by hitting a walk-off home run to
Pablo Sandoval in historically bad slump for Giants
When the San Francisco Giants signed Pablo Sandoval in July, both parties were hoping that a change of scenery would revive Kung Fu Panda's career. That has not been the case.
Sandoval has been
Pablo Sandoval admits he never should have left Giants
After two and a half disastrous years in Boston, Pablo Sandoval is back with the San Francisco Giants, and is looking back on the events that led him there.
In an article written for the Players&#821
Pablo Sandoval cheered in return to Giants lineup (Video)
Pablo Sandoval made his return to the Giants lineup and was greeted warmly when introduced at AT&T Park in San Francisco.
Sandoval signed a minor league deal with the Giants after being released
Pablo Sandoval apologizes for comments about Giants
Pablo Sandoval is back with his original organization, and he is looking to get back in the good graces of the team's fan base. To that end, he apologized for comments he made upon joining the
Pablo Sandoval appears at AT&T Park after signing with Giants
Pablo Sandoval is back with the team where he enjoyed the most success.
Sandoval has chosen to sign a minor-league deal with the San Francisco Giants, days after being released by the Boston Red Sox,
Report: Giants will sign Pablo Sandoval
Pablo Sandoval is going home again.
According to Jon Heyman of FanRag Sports, the San Francisco Giants will sign the third baseman, who was designated for assignment last week by the Boston Red Sox.
Pablo Sandoval would reportedly 'love' to return to Giants
Pablo Sandoval's tenure in Boston was an unmitigated disaster, and now that it's over, he reportedly wants to return to a place where he knows he's been a success.
According to Jon
Pablo Sandoval designated for assignment by Red Sox
The Pablo Sandoval era in Boston may finally be over.
On Friday, the Red Sox announced that they have designated Sandoval for assignment. It's highly unlikely that any team will pick up the two
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Hackett, 33, is the founder and president of SONset Friday Entertainment, a faith-based production company that he owns and operates with his wife Adanna. Hackett is a Christian actor, filmmaker and entertainer whose stage plays and movies are making waves in the urban community and touching hearts across racial divides.
"Love Different" is about Lindsay Walker (played by Jenn Gotzon), who is a Caucasian woman from a small town populated by white people. She is hired by an African-American consulting firm and is surrounded by black people for the first time. It's a culture shock for Lindsay, so the boss gives an African-American co-worker, Neque Campbell (played by Hackett), the task of helping Lindsay understand African-American culture.
Kevin Fredericks plays Professor Black. The professor teaches a class that educates white people on how to understand black people.
"It would be funny if that was a real thing people did and taught people that 'everybody doesn't want to steal your purse' and 'all black people don't like fried chicken.' Those stereotypes seem silly, but people believe them and they're going to base their reactions on them," Fredericks said.
Fransha' described what it's like working with Hackett.
"Love Different" was produced in three months and filmed in about 20 different locations in Maryland, with one location being within Prince George's County at the Dutch Country Farmers Market in Laurel. Hackett also stars in "Love Different." His ability to wear more than one hat impressed his actors.
Gotzon said Hackett has the ability of transcending the genres between faith, family and urban cultures. She rated "Love Different" as a family-friendly movie that mainstream audiences and urban market followers of Tyler Perry will love. Gotzon voiced her hope for how "Love Different" will be received by audiences.
The release date for "Love Different" is yet to be announced. Meanwhile, people can learn more about the movie by visiting the movie's official website, www.LoveDifferentTheMovie.com, choosing to "like" the movie's fan page (https://www.facebook.com/LoveDifferentTheMovie/), and following Hackett's production company on Twitter @SONsetFriday.


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Jen Taylor,
Colleen Jenny and Theresa Wagner use Applied Behavorial Analysis, a system of repetition and rewards, to help combat autism.
Signs of Trouble
"If you've met one person with autism," goes an oft-repeated saying among autism advocates, "you've met one person with autism."
In other words, autism manifests itself in a variety of ways, and no two people on the autism spectrum will have precisely the same set of symptoms. But there are certain cardinal signs of the disorder, says pediatrician Joseph Stegman, founder of Developmental & Behavioral Pediatrics of the Carolinas in Concord.
Chief among them are lagging socialization skills. A baby with autism might not respond to his name, make strong eye contact or show shared interest in an object or activity—known as "joint attention."
Delays or regression in language skills are also common in autistic children, and restrictive, repetitive behaviors—such as rocking or hand flapping—are often seen.
Even with increasing awareness of the symptoms, Stegman says he hears of too many cases in which parents concerned about autism were put off by a well-meaning pediatrician, and lost valuable time during which their child could have started treatment.
"It's very hard to tell a parent that there is something wrong with their child, so some doctors take a wait-and-see approach longer than they should," says Stegman.
It can take months to get an appointment with a specialist qualified to diagnose autism, and Stegman says parents shouldn't hesitate to ask their child's pediatrician for a referral to a speech or occupational therapist, who can start working with a child even before he or she gets an official autism diagnosis.
For more information, check out the Autism Society of America's "Autism 101" online course, at www.autism-society.org.
Who's Helping
Garr Christian Academy
Cure Autism Now. Those are two popular rallying cries in the fight against the developmental disability that has more than 1.7 million people in its grip. One Charlotte school is attempting to add another verb to the growing autism lexicon: Garr. As in Garr Autism Now. As in Garr Christian Academy, an east Charlotte private school where about thirty autistic children are being educated amongst the school's 250 or so typically developing preschool through eighth grade students. Through a system called Applied Behavioral Analysis, teachers use repetition and rewards to teach desired behavior. "We're teaching them that their language will get them what they want, what they need," says Garr ABA director Theresa Wagner.
ABA is highly regarded as a method for teaching kids with autism, but it is tremendously costly. In Garr's four classrooms, there is one co-teacher for every two students, as well as one lead teacher for the whole class.
ABA generally isn't offered in its purest form in public schools, though ABA principles are often used in public school special education programs. Wagner, who started the Garr ABA program four years ago along with program consultant Wyndie Stitt, says it has a waiting list of about thirty-five children whose families are willing to pay tuition and fees of about $20,000 a year, which is supplemented by the school's extensive fundraising efforts. Wagner says families have moved here from other states so their children could learn at Garr.
Autism is a complex neurobiological disorder that impairs a person's ability to communicate with and relate to others, according to Autism Speaks, a group that supports autism research and advocacy. A person diagnosed with autism is said to be somewhere on the autism spectrum, from mild to severe.
Since the 1990s, the number of autism cases has skyrocketed from one in every 5,000 children to one in every 150 children. It's unclear how much of that jump is attributable to increased awareness and diagnosis of autism, but there's a slew of alarming autism statistics to share:
In the Charlotte-Mecklenburg school system, one in seventy-three children are currently diagnosed with autism spectrum disorder.
It is estimated that as many as 30,000 people in North Carolina are living with autism spectrum disorder. In the U.S., more than 500,000 people under the age of twenty-one have autism.
Researchers have found no statistical link between autism and socioeconomic status, race or ethnicity, but there does appear to be a gender component. Boys are four times as likely as girls to be diagnosed with autism.
This article appears in the July 2008 issue of Charlotte magazine.
Categories: Feature, Health + Beauty > Features


Learn from the Comfort of Home!
You want to learn everything you can, so that you can have the relationship of your dreams, right?
The only problem is, you've got no time!
How on earth do you fit it all in?
Here's the solution to your problem: self-paced learning, all available on your schedule!
If you've got any questions, email: karen@theheartmatters.com or call: (978-557-9993), and we'll chat!


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Stars Bio Point
Home » Rakhi Sawant Age, Height, Weight, Career, Net Worth, Husband, Affairs & Bio
Rakhi Sawant Age, Height, Weight, Career, Net Worth, Husband, Affairs & Bio
In India, an Indian dancer, model, and actor, Rakhi Sawant, was born on the 25th of November, 1978. Rakhi Sawant has a real name as Neeru Bheda, although she changed her name for the industry. She is also recognized with the names like Controversy queen and Drama queen due to her everyday dissension and hype in the media. Here we talking about Rakhi Sawant age, height, career, family, weight, movies, lifestyle, affairs, and more:
Rakhi Sawant Bio:
Real Name Neeru Bheda
Nickname Drama Queen, Controversy Queen
Date Of Birth 25 November 1978
Birthplace Mumbai, Maharashtra, India
Hometown Mumbai, Maharashtra, India
School Goklibai High School, Mumbai
University/ College Mithibai College, Mumbai
Qualification Unknown
Religion She was born into a Hindu Family, But she follows Christianity
Food Habit Non-Vegetarian
Political Party BJP
Address B2/501, Serenity Complex, New Link Road, Oshiwara, Andheri (West) Mumbai
Rakhi Sawant Physical Statics & More:
Weight (in Pound) 132 lbs
Weight (in KG) 60 kg
Height (in Meter) 1.60 m
Height (in Feet) 5'3″ Inches
Bra Size 36 Inches
Hip Size 36 Inches
Waist Size 28 Inches
Rakhi Sawant Family & Personal Life:
Husband Ex-husband: Ritesh Singh
Boyfriend Deepak Kalal
Step-father Anand Sawant (Police Constable)
Mother Jaya Bheda
Brother Rakesh Sawant ( Film Director)
Sister Usha Sawant (Actress)
Son Unknown
Daughter Unknown
Rakhi Sawant Career & Net Worth:
Profession Politician, Actress, Dancer
Debut Agnichakra (1997)
Salary 2-3 Lakh
Rakhi Sawant Favorite Things:
Hobbies Dancing
Favorite Actors Shah Rukh Khan, Ranveer Singh
Favorite Actress Priyanka Chopra, Deepika Padukone, Sonakshi Sinha
Favorite Food Grilled Chicken, Salad
Favorite Colour Blue, Black
Favorite Destination Switzerland
Rakhi Sawant Social Media:
Rakhi is a model and dancer who appeared in many Hindi movies and television shows, and she has also been a television talk show host. As well as Hindi movies, Rakhi Sawant also appeared in a few Marathi, Kannada, Tamil, Telugu, and Odia movies. In its first season, she was also a participant in India's most controversial reality show, known as Big Boss. Her fame depends on defaming, controversies, and public stunts; however, she was an adultery symbol throughout her career. Rakhi's mother, Jaya Bheda, and her biological father, Anand Sawant, her father was police constable at the police station.
Rakhi's mother, Jaya, gave the name of her second husband to her three kids from her first husband. Rakhi has two siblings' one brother and a sister, her brother, Rakesh Sawant, is a film director, while her sister, Usha Sawant, is a former actress. Due to her poor financial family situation, Rakhi hardly managed to go to school. She lately converted to Christianity. Sawant made her first debut in the Hindi film industry with the movie Agnichakr.' Then she played many other small roles and a couple of item numbers in Bollywood movies Ye Raaste Hain Pyaar Ke, Joru Ka Ghulam, and Jis Desh Mein Ganga Rehta Hain. In 2003, Sawant auditioned around four times for an item number in a Bollywood movie named Chura Liyaa Hai Tumne.
This was her breakthrough item song known as 'Mohabbat hai Mirchi' made under the music director Himesh Reshammiya. She played small roles in movies like Main Hoon Na and Masti. She gained a different name in the industry with her Music video for the song 'Pardesiya' by DJ Hot Remix. The year 2006 was the year of the biggest controversy for Rakhi Sawant and Mika Singh. After one year, Sawant decided to make a singing debut, and the album 'Super Girl' was not a good result; the album was produced by Venus Records & Tapes Pvt. Ltd. She often hosts reality shows and sometimes appears as a judge and contestant; according to her, she is a regular stage performer and would love to continue with this in the future.
She also performed comedy acts along with Bollywood actors Ranbir Kapoor and Shah rukh khan at the 57th Filmfare awards. Sawant also performed a dance act in a few award ceremonies. Rakhi Sawant appeared in the leading role in the thriller movie 'Ek Kahani Julie Ki.' She played a comedy role in the comedy fiction series on television known as 'Bhaag Bakool Bhaag.' She played small roles in many Hindi movies and other languages movies in India. She performed in various music videos, including Jhoomka Gira Re Remix Sweet Honey Mix, Kajra Nite Remix, Tu Dissda, Haadsa, Bhoot, Jhagde, and Chappan Churi.
In 2014, Sawant announced that she plans to contest Lok Sabha Election 2014 as an independent candidate from North-West Mumbai. In the same year, on 28th March, she founded her political party Rashtriya Aam Party. However, the election commission did not assign a party symbol; Sawant expected the party symbol should be 'Green Chilli.' Her party's fundraisers and office bearers were local businessmen from Oshiwara. Unfortunately, she just got 15 votes from the North-West Mumbai constituency. Later Rakhi Sawant joined the RPI party after resigning from her founded Rashtriya Aam Party. She is now serving the party in the post of State vice president and working as president of the woman's wing.
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