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EECP Therapy
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Arterial Duplex
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Cardiology Providers
M. Akram Paracha, MD, FACC, FSCAI, FSVM
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Vascular Providers
Home / Cardiology Clinic / Providers / M. Akram Paracha, MD, FACC, FSCAI, FSVM
After earning his medical degree and completing his internship at Dow University of Health Sciences in Pakistan, Dr. Paracha moved to the U.S. and completed his Residency in Internal Medicine at Michigan State University. Following his residency, Dr. Paracha completed Fellowship training in Critical Care Medicine at Mt. Sinai Medical Center in New York and Wayne State University in Detroit.
Dr. Paracha remained at Wayne State's Detroit Medical Center to practice critical care medicine and serve as an Assistant Professor. While training pulmonary and critical care specialists, he developed a keen interest in Critical Care Cardiology. He went on to complete Fellowship training in General and Interventional Cardiology and Vascular Medicine at Wayne State. To continue his career, Dr. Paracha chose the Fayetteville area, where he felt there was a need for specialized vascular and cardiac services.
Since 2002, Dr. Paracha has been providing comprehensive cardiology and vascular services for patients in Fayetteville and surrounding areas. Over the past decade – since he developed Valley Cardiology's Vascular Clinic – Dr. Paracha has provided much-needed care to promote wound healing and prevent limb loss in patients with Critical Limb Ischemia (CLI). The Vascular Clinic now has three locations (Fayetteville, Lumberton, and Lillington) that offer the most advanced, state-of-the-art care for patients in the region who suffer from Peripheral Arterial Disease (PAD), venous disease and lymphedema.
Dr. Paracha has special interests in interventional cardiology and vascular medicine, and he is Board Certified in Cardiovascular Disease, Interventional Cardiology, Vascular Medicine and Venous & Lymphatic Medicine. He is a Fellow of the American College of Cardiology, the Society for Cardiovascular Angiography and Interventions, and the Society for Vascular Medicine.
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text:
Liberty extends home win streak to 17 with win over FGCU
Published Saturday, Feb. 1, 2020, 10:48 pm
Liberty set a school-record, winning its 17th straight home game at the Vines Center Saturday night, with a resounding 61-46 win over Florida Gulf Coast.
The Flames improve to 21-3 this season and 7-2 in the ASUN Conference while FGCU drops to 7-17 overall and 4-5 in conference.
Liberty forced 12 turnovers in the first half, which led to 18 points for the Flames, while FGCU was unable to score any off Liberty's four turnovers.
Liberty would go into the break with a 33-14 lead.
The Flames shot 50 percent from the field in the second half, led by Caleb Homesley's eight points, three rebounds and a pair of steals all in the second half. FGCU's Jalen Warren led all scorers in the second half with 12 points but Liberty's starters would do most of the damage in the second half, scoring 23 of Liberty's 28 points.

redpajama_set_name: RedPajamaCommonCrawl


text:
'In the Heat of Night' actress Stewart will be keynote for fall 2019 joint commencement
3 years ago HBCU Staff
(JACKSON, Miss.) – Actress and JSU alum Tommie "Tonea" Stewart of "In The Heat of The Night" fame will be the fall 2019 Graduate/Undergraduate Commencement speaker at 10 a.m. Friday, Dec. 6, in the Lee E. Williams Athletics and Assembly Center.
Stewart earned her undergraduate degree in speech and theater from Jackson State University in 1969. Later she studied at the University of California at Santa Barbara, receiving a master's degree in theater arts. She was the first African American woman to receive a doctorate in theater arts from Florida State University. In addition, she studied under well-known coaches such as Beah Richards, Frank Silvera and Joseph Papp.
In addition, she is a retired tenured professor and was dean of the College of Visual & Performing Arts at Alabama State University.
The former Miss JSU is best known for her role as "Aunt Etta Kibbe" on "In The Heat of the Night." As well, she played "Old Cora" in an episode of "American Horror Story" on the FX Channel, which starred Angela Bassett and Kathy Bates. The acclaimed actress has been in big-screen productions, including "A Time to Kill," which earned her an NAACP Image Award nomination, and in "Mississippi Burning."
Last year, Stewart was featured in a Netflix drama based on true events about internationally renowned pastor Carlton Pearson, who risked everything after questioning church doctrine and being branded a modern-day heretic.
Outside of her film work, Stewart has spent more than 25 years operating a summer youth camp for young people seeking professional training in the performing arts.
Tags: Actress, Commencement, FALL, keynote, Theatre
Previous Fisk University promotes Jens Frederiksen to Senior Vice President for Institutional Advancement and Enrollment.
Next DSU COMMENCEMENT TO FEATURE JOSHUA DuBOIS, FORMER OBAMA WHITE HOUSE OFFICIAL


What great news! I am very much looking forward to learning more about this topic!
For so long, we have all been taught that as you age from a teen into a young adult, your brain STOPS making new neurons. This has always been a grim concept to me (as I am past the oft-cited 26 year mark), I abhor the thought that we don't get more chances at dramatic change. This was never to say that an old dog couldn't learn a new trick; however the idea was just that…more behavioral than anything. This TED talk sheds light on new research that is discovering that the aging adult brain does indeed create new neurons, notably in the hippocampus. New neurons in the hippocampus = improved memory functioning and MOOD.
Unfortunately for some out there (not naming names…you know who you are…) this is another scenario where it is imperative that you sleep well, eat well, and exercise in order to reap the benefits. Chronic stress, high sugar diets and alcohol all decrease the neurogenesis in your hippocampus.


The Innu (Naskapi) shirt, replete with subtle mends, was painted by a female artist in collaboration with a hunter engaged in the holy task of pursuing caribou. The coat's designs, reflecting the hunter's dreams, symbolize reciprocity between humans and animals. The silhouettes of both the coat and the Eastern Dakota child's jacket reflect how European presence was integrated and remixed to create new indigenous expressions. [See also 44.593].
The images on this website can enable discovery and collaboration and support new scholarship, and we encourage their use. This object is in the public domain (CC0 1.0). This object is Child's Jacket with the accession number of 1988.112.10. To request a higher resolution file, please submit an online request.


Home → Parenting → Hungry?
"Never stop for groceries when you're hungry." Have you ever heard that statement?
It's founded on studies that show that impulse buying results in greater purchases and more consumption of high-fat, high-calorie, and high-cost foods. In addition, people who shop when they are hungry are more likely to purchase things they don't need or things they would not normally buy.
The same can be true in other areas of our lives. Consider for a moment what happens when we are spiritually malnourished. Rather than feasting on the Word of God which promises to completely satisfy, we choose to consume the empty things of the world, leaving us wanting. Also, we can make decisions that come at a cost to us personally because of the resulting consequences which are often difficult to reverse. In addition, people who are spiritually hungry are more likely to indulge in things that reflect the flesh rather than God's best for them. They do things they wouldn't do if lead by the Spirit.
The Bible refers to Jesus as "The Bread of Life". Psalm 107:9 says "He satisfies the thirsty and fills the hungry with good things." Are you allowing yourself to go spiritually hungry or are you being consistently filled with the Word of God?
Do pets really resemble their owners?


text:
Find: nice piece on android fragmentation
While old apple devices receive regular updates because they remain in stores a long time, old android devices don't, because they are gone so quickly.
Seems like an opportunity to create a superior experience for the right carrier/manufacturer.
What happened to the Android Update Alliance?
Android introduced Jelly Bean at I/O earlier today, but how many existing devices will see the update?
Dan Goodin, Ars Technica
Google's Android keynote this morning was packed with announcements, most prominent among them the introduction of Jelly Bean, the next version of the Android mobile operating system. While it looks to be a solid update to last year's Ice Cream Sandwich, there's a big question that always looms large over the announcement of any new Android version: these features look nice and all, but will my device ever be upgraded?
At last year's Google I/O, the company announced the Android Update Alliance, an initiative through which Google would work with its partners to ensure that Android phones and tablets would receive updates for at least 18 months after their introduction. This much-ballyhooed announcement wouldn't have done much about the extreme diversity of hardware in the Android ecosystem, but it would have helped reduce the growing software fragmentation issues that the platform was facing.
There was just one problem: the Android Update Alliance hasn't really been mentioned since, including in today's keynote.


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

Over the last decade, there has been an increasing interest of the astrophysics community on highly magnetized white dwarfs (HMWDs) both from the theoretical and observational points of view. These sources constitute at least 10\% of the white dwarfs (WDs) if observational biases are considered~\citep{2007ApJ...654..499K}. These WDs with surface magnetic fields raging from $10^6$~G to $10^9$~G have  been confirmed by the recent results of the Sloan Digital Sky Survey (SDSS) \citep{2009A&A...506.1341K,2010AIPC.1273...19K,2013MNRAS.429.2934K,2015MNRAS.446.4078K}. Besides their high magnetic fields, most of them have been shown to be massive, and responsible for the high-mass peak at $1~\textrm{M}_\odot$ of the WD mass distribution; for instance: REJ 0317--853 has $M \approx 1.35~\textrm{M}_\odot$ and $B\approx (1.7$--$6.6)\times 10^8$~G \citep{1995MNRAS.277..971B,2010A&A...524A..36K}; PG 1658+441
has $M \approx 1.31~\textrm{M}_\odot$ and $B\approx 2.3\times 10^6$~G \citep{1983ApJ...264..262L,1992ApJ...394..603S};
and PG 1031+234 has the highest magnetic field $B\approx 10^9$~G \citep{1986ApJ...309..218S,2009A&A...506.1341K}. The existence of ultra-massive WDs has been revealed in several studies~\citep{2005A&A...441..689A,2007A&A...465..249A,2013MNRAS.430...50C,2013ApJ...771L...2H,2017MNRAS.468..239C,2019A&A...625A..87C,10.1093/mnras/sty3016,2018MNRAS.480.4505J}.

Typically, WDs rotate with periods of days or even years. Recently, a WD pulsar known as AR Scorpii was discovered with a period of $1.97$ min, emitting radiation in a broad range of frequencies, typically of neutron star (NS) pulsars \citep{2016Natur.537..374M}. The spindown power is an order of magnitude larger than the observed luminosity (dominated by the X-rays), which, together with an absence of obvious signs of accretion, suggests that AR Sco is primarily rotation-powered. The AR Sco's broadband spectrum is characteristic of synchrotron radiation, requiring relativistic electrons, possibly originated from the neighborhood of the WD and accelerated to almost the speed of light~\citep{2017JPhCS.861a2005L}. Furthermore, other sources have been proposed as candidates of WD pulsars. A specific example is AE Aquarii, the first WD pulsar identified, with a short rotation period of $P=33.08$~s~\citep{2008PASJ...60..387T} and spinning down at a rate $P=5.64\times 10^{-14}$~s/s. The rapid braking of the WD and the nature of hard X-ray pulses detected with SUZAKU space telescope~\citep{2008AdSpR..41..512T} can be explained in terms of spin-powered pulsar mechanism~\citep[see][]{1998A&A...338..521I}. On the other hand, the X-ray Multimirror Mission (XMM) - Newton satellite has observed a WD faster than AE Aquarii. Mereghetti et al.~\citep{2009Sci...325.1222M} showed that the X-ray pulsator RX J0648.0-4418 is a massive WD with mass $M=1.28M_\odot$ and radius $R = 3000$ km~\citep[see][for derived mass-radius relations for massive oxygen-neon WDs that predict this radius]{refId0,Althaus2007}, with a very fast spin period of $P = 13.2$~s, that belongs to the binary system HD 49798/RX J0648.0-4418. More recently, \cite{2020ApJ...898L..40L} report on XMM-Newton observations that reveal CTCV J2056-3014 to be an X-ray-faint intermediate polar harboring an extremely fast-spinning WD with a coherent 29.6 s pulsation.

Notwithstanding, several currently studies of fast-rotating and magnetized WDs have been done, in particular the one involving WD pulsars in an alternative description for Soft Gamma Repeaters (SGRs) and Anomalous X-Ray Pulsars (AXPs) \citep[see][and references therein]{Malheiro/2012,Coelho/2014,2016IJMPD..2541025L,2016JCAP...05..007M, 2017MNRAS.465.4434C}. From this perspective, a canonical spin-powered pulsar model can explain the process of energy emission released by dipole radiation in a WD, since they share quite similar aspects \citep{Usov/1988,Coelho/2014}. In addition, these sources could also be candidates for GW emission, since the huge magnetic field can deform the star in a non-symmetrical way, thus generating a variation in the quadrupolar moment of the star.

In a second proposed scenario, that of a WD pulsar, the optical/IR data are explained by the WD photosphere and by a disk~\citep{2013ApJ...772L..24R}.  Recently, a new  scenario has been  proposed to  explain the spectral energy distribution (SED) of 4U 0142+61, from mid-infrared up to hard X-rays~\citep{Sarah2019}. In this model, the persistent emission comes from an accreting isolated magnetic WD surrounded by a debris disk, having gas and dusty regions.

On the other hand, direct observations of GWs have recently been made by LIGO and Virgo. The first event was detected in 2015 by LIGO \citep{ABBOTT/2016}. This event, named GW150914, came from the merging of two black holes of masses $ \sim  35.6\,\rm{M}_{\odot}$ and $30.6\,\rm{M}_{\odot}$ that resulted in a black hole of mass $ \sim  63.1\,\rm{M}_{\odot}$. Thereafter, LIGO in collaboration with Virgo observed 9 more such events \citep{ABBOTT/2017a,ABBOTT/2017c,ABBOTT/2017b,Abbott_2019}. In addition, the event GW170817 reports the first detection of GW from a binary NS inspiral \citep{abbott2017d}.
All GW detections are within a frequency band ranging from $10$ Hz to $1000$ Hz, which is the operating band of LIGO and Virgo. As is well known, there are proposed missions for lower frequencies, such as LISA \citep{AMARO/2017,cornish2018}, whose frequency band is of $(10^{-4}-0.01)$ Hz, BBO \citep{harry/2006,yagi2011} and DECIGO \citep{kawamura/2006,yagi2017} in the frequency band ranging from $0.01$ Hz to $10$ Hz.

Different  possibilities  of  generation  of continuous GWs have already been proposed~\citep[see e.g.,][and references therein]{1996A&A...312..675B,2016EPJC...76..481D,2016ApJ...831...35D,2016JCAP...07..023D,10.1093/mnras/stx2119,2017EPJC...77..350D,2017ApJ...844..112G,Schramm/2017,2018EPJC...78..361P,2019arXiv190600774D}. More recently, Kalita and Mukhopadhyay \citep{2019MNRAS.490.2692K} shows that continuous GWs can be emitted from rotating magnetized WDs and will possibly be detected by the upcoming GW detectors such as LISA, DECIGO and BBO. The main goal of the present paper is to extend our previous study \citep{10.1093/mnras/staa205} in which we investigated the gravitational radiation from three fast-spinning magnetized WDs, which have high rotations (a few seconds to minutes) and  huge magnetic fields ($10^{6}$ G to $\sim 10^{9}$ G), considering two emission mechanisms: matter accretion and magnetic deformation. In both cases, the GW emission is generated by asymmetry around the rotation axis of the star due to accumulated mass in the magnetic poles and due to the intense magnetic field, respectively. Here, we explore the magnetic deformation mechanism of gravitational radiation emission in SGRs/AXPs as fast-spinning magnetized WD.

This paper is organized as follows. In Sec.~\ref{sec:5}, we present the aspects
of the model used to explain SGRs/AXPs. In Sec.~\ref{sec:6}, we describe the mechanism of GW emission by deriving the equations for the gravitational amplitude and luminosity. In Sec.~\ref{sec:9} we present and discuss the calculations applied to SGRs/AXPs described as WD pulsars. Finally, in Sec.~\ref{sec:13} we summarize the main conclusions and remarks.

\section{SGRs/AXPs as white dwarf pulsars }
\label{sec:5}

SGRs and AXPs are a special class of pulsars that present distinct characteristics from radio pulsars and X-ray pulsars (see Table \ref{tabla:SGR/AXP}). They are described by the magnetar model, where they are considered strongly magnetized NS with magnetic field of the order of $10^{12} - 10^{15}$ G. Also, these objects are known as very slow rotating pulsars comparing to ordinary pulsars, with rotational periods in the range of $P \sim 2-12$ s and a high spindown rate of $\dot{P} \sim 10^{-13} - 10^{-10}$~s/s~\citep[see][and references therein]{Olausen/2014}\footnote{For information  about the SGRs/AXPs, we refer the reader to the McGill University's online catalog available at: \url{http://www.physics.mcgill.ca/~pulsar/magnetar/main.html}}.

\begin{table*}
\begin{center}
\caption{Observational quantities taken from McGill Pulsar Group's online catalog for confirmed SGRs/AXPs: Period ($P$). spindown ($\dot{P}$), observed luminosity ($L_{X}$) and distance to the source ($r$).}
\vskip0.3cm
\begin{tabular}{lcccc}
\hline
\textbf{SGR/AXP} & \begin{tabular}[c]{@{}c@{}}$P$\\ (s)\end{tabular} & \begin{tabular}[c]{@{}c@{}}$\dot{P}$\\ ($10^{-11}$ s/s)\end{tabular} & \begin{tabular}[c]{@{}c@{}}$L_{X}$\\ ($10^{33}$ erg/s)\end{tabular} & \begin{tabular}[c]{@{}c@{}}$r$\\ (kpc)\end{tabular} \\ \hline
CXOU J010043.1-721134 & 8.020392 & 1.88 & 65 & 62.4 \\
4U 0142+61 & 8.688692 & 0.2022 & 105 & 3.6 \\
SGR 0418+5729 & 9.078388 & 0.0004 & 0.00096 & 2 \\
SGR 0501+4516 & 5.76207 & 0.594 & 0.81 & 2 \\
SGR 0526-66 & 8.0544 & 3.8 & 189 & 53.6 \\
1E 1048.1-5937 & 6.457875 & 2.25 & 49 & 9 \\
1E 1547.0-5408 & 2.072126 & 4.77 & 1.3 & 4.5 \\
PSR J1622-4950 & 4.3261 & 1.7 & 0.44 & 9 \\
SGR 1627-41 & 2.594578 & 1.9 & 3.6 & 11 \\
CXOU J164710.2-455216 & 10.61064 & $\leqslant$ 0.04 & 0.45 & 3.9 \\
1RXS J170849.0-400910 & 11.00502 & 1.9455 & 42 & 3.8 \\
CXOU J171405.7-381031 & 3.825352 & 6.40 & 56 & 13.2 \\
SGR J1745-2900 & 3.763638 & 1.385 & $\leqslant$ 0.11 & 8.3 \\
SGR 1806-20 & 7.54773 & 49.5 & 163 & 8.7 \\
XTE J1810-197 & 5.540354 & 0.777 & 0.043 & 3.5 \\
Swift J1822.3-1606 & 8.437721 & 0.0021 & $\leqslant$ 0.00040 & 1.6 \\
SGR 1833-0832 & 7.565408 & 0.35 & ... & $\leqslant$ 10 $^{a}$ \\
Swift J1834.9-0846 & 2.482302 & 0.796 & $\leqslant$ 0.0084 & 4.2 \\
1E 1841-045 & 11.78898 & 4.092 & 184 & 8.5 \\
J185246.6+003317 & 11.55871 & $\leqslant$ 0.014 & $\leqslant$ 0.0060 & 7.1 \\
SGR 1900+14 & 5.19987 & 9.2 & 90 & 12.5 \\
SGR 1935+2154 & 3.245065 & 1.43 & ... & $\leqslant$ 10 $^{b}$ \\
1E 2259+586 & 6.979043 & 0.0483 & 17 & 3.2 \\ \hline
\end{tabular}

$^{a}$see \cite{esposito2011}. $^{b}$ see \cite{kozlova2016}.

\label{tabla:SGR/AXP}
\end{center}

\end{table*}

Recently, three SGRs with low magnetic field ($B\sim 10^{12}-10^{13}$~G) have been observed, namely, SGR 0418+5729, Swift J1822.3-1606 and 3XMM J185246.6+00331. These new discoveries open the question concerning the nature of SGRs/AXPs, emerging alternative scenarios, in particular the WD pulsar model. These astronomical observations have based an alternative description of the SGRs/AXPs, which are modeled as rotating highly magnetized and very massive WDs~\citep[see][for further details]{Malheiro/2012,Coelho/2014,2017MNRAS.465.4434C}. From this perspective, a canonical spin-powered pulsar model can explain the process of energy emission released by a dipole radiation in a WD, since they share quite similar aspects~\citep[see][]{Usov/1988}. In this new description, several observational properties are explained as a consequence of the large radius of a massive WD that manifests a new scale of mass density, moment of inertia, rotational energy, and magnetic dipole moment in comparison with the case of NSs~\citep[see e.g.,][and references therein]{Coelho/2014,2016IJMPD..2541025L}.

In the canonical pulsar model, a rotating star with magnetic dipole moment misaligned to the axis of rotation converts rotational energy into electromagnetic energy. Thus, the system emits radiation due to the variation of the magnetic dipole and the pulsar rotation becomes slower. If we consider that all rotational energy loss is converted to electromagnetic energy, we can infer the magnetic field strength on the star's surface, $B_{s}$, as a function of the period $P = 1/f_{rot}$ and its derivative $\dot{P} = dP/dt$ \citep[see, e.g.,][]{Coelho/2014}

\begin{equation}
    B_{s}\sin \phi =  \left ( \frac{3c^{3} I}{8\pi^{2} R^{6} }P \dot{P}{ } \right )^{1/2},
    \label{CMs}
 \end{equation}

\noindent where $I$ is the moment of inertia, $R$ is the star radius, $\phi$ is the unknown angle between the rotation and magnetic dipole axes and $c$ is the speed of light.

Note that because the moment of inertia values for a NS and a WD are different, the magnetic fields required in each model are also different. For example, for a NS with mass $M = 1.4 M_{\odot }$ and radius $R = 10^{6}$ cm, the magnetic field on the star's surface are in the range of $10^{13} - 10^{15}$ G. For a very massive WD with mass $M = 1.4 M_{\odot }$ and radius $R \sim 10^{8}$~cm \citep[see, e.g,][]{Coelho/2014}, the magnetic field has smaller values and is in a range around $10^{9} - 10^{11}$ G, comparable to the inferred values of known HMWDs \citep{2009A&A...506.1341K,2010AIPC.1273...19K,2013MNRAS.429.2934K,2015MNRAS.446.4078K}.
Thus, these values of mass and radius generate a moment of inertia $I\simeq 1.1\times 10^{49}$ $\rm g.cm^2$. These results clearly show that the scale of the magnetic field in WD is $10^4$ times smaller than for NSs.

In addition, since the high magnetic field can deform the star in a non-symmetrical way, new values for the  ellipticity are expected and, consequently, new values for the GW amplitude as well (see section \ref{sec:6}).
In the next section, we describe the magnetic deformation mechanism and deduce the GW amplitude and luminosity emitted in this process.

\section{Magnetic deformation mechanism: basic equations}
\label{sec:6}

WDs might generate GWs whether they are not perfectly symmetric around their rotation axes. This asymmetry can occur, for example, due to the huge dipole magnetic field that can make the star become oblate \citep[see, e,g,][]{chandrasekhar1953s}. In this work, we analyze the emission of gravitational radiation from SGRs/AXPs as fast-spinning magnetized WDs by this mechanism.

Thus, in this section we consider the deformation of the WDs induced by their own huge magnetic fields. Due to the combination of magnetic field and rotation, a WD can become  triaxial, presenting therefore a triaxial moment of inertia. In order to investigate the effect arising from the magnetic stress on the equilibrium configuration of the stars, let us  introduce  the equatorial ellipticity, defined as follows \citep[see, e.g.,][]{shapiro/2008,maggiore/2008}

\begin{equation}
  \epsilon = \frac{I_{1} - I_{2}}{I_{3}}.
 \label{elipticidade}
\end{equation}

\noindent where $I_{1}$, $I_{2}$ and $I_{3}$ are main moments of inertia with respect to the ($x$, $y$, $z$) axes, respectively.

If the star rotates around the $z-$axis, then it will emit monochromatic GWs with a frequency twice the rotation frequency, $f_{rot}$, and amplitude given by \citep[see, e.g.,][]{shapiro/2008,maggiore/2008}

\begin{equation}
   h_{df} = \frac{16 \pi^{2} G}{c^{4}}  \frac{I_{3} f_{rot}^{2}}{r} \, \epsilon,
\label{Ampdef2}
\end{equation}

\noindent and the rotational energy of the star decreases at a rate given by \cite[see, e.g.,][]{shapiro/2008,maggiore/2008}

 \begin{equation}
   L_{GW_{df}} = - \frac{2^{11}  \pi^{6} }{5} \frac{G}{c^{5}} I_{3}^{2} \epsilon^{2} f_{rot}^{6}.
\label{Lumidef1}
\end{equation}

On the other hand, recall that the ellipticity of magnetic origin can be written as follows~\citep[see, e.g.,][]{1996A&A...312..675B,2000A&A...356..234K,2006A&A...447....1R}

\begin{equation}
\epsilon = \kappa \frac{B_{s}^{2} R^{4}}{G M^{2}} \sin^2{\phi},
    \label{excentridade}
\end{equation}

\noindent where, as before, $B_{s}$ is the magnetic field strength on the star's surface, $R$ and $M$ are, respectively, the radius and mass of the star, $\phi$ is the angle between the rotation and magnetic axes, whereas $\kappa$ is the distortion parameter, which depends on the magnetic field configuration and equation of state (EoS) of the star. It is worth mentioning that as the magnetic field of the SGRs/AXPs is inferred from the spindown rate of the star, where it is considered that all rotational energy loss is converted into electromagnetic energy [see Eq.~(\ref{CMs})], care must be taken when using these field values to calculate an additional GW spin-down torque. In fact, in the next section, we show that this procedure is safe and that only a small fraction of the total energy loss goes to GWs.

To proceed, substituting this last equation into Eqs.~(\ref{Ampdef2}) and (\ref{Lumidef1}) and considering $I_3 = 2MR^{2}/5 $, one immediately obtains that

\begin{equation}
   h_{df} = \frac{32 \pi^{2} }{5 c^{4}}  \frac{R^{6} f_{rot}^{2}}{r M} \kappa (B_{s}\sin{\phi})^{2},
\label{Ampdef3}
\end{equation}
and
\begin{equation}
   L_{GW_{df}} = - \frac{2^{13} \pi^{6} }{5^3 c^{5}} \frac{ R^{12} f_{rot}^{6}}{G M^{2}}\kappa^2 (B_{s}\sin{\phi})^{4}.
\label{Lumidef2}
\end{equation}

Thereby, we find equations for the gravitational luminosity and the GW amplitude which depend on the rotation frequency and the magnetic field strength.

A very interesting equation can be obtained by substituting Eq.~(\ref{CMs}) into Eq.~(\ref{excentridade}), namely
\begin{equation}
\epsilon = \frac{3}{20 \pi^2}\frac{c^{3}}{G M} P{\dot P}\kappa,
    \label{excentridade2}
\end{equation}

\noindent which is independent of the angle $\phi$.

Consequently, by substituting Eq.~ (\ref{excentridade2}) into
Eqs.~(\ref{Ampdef3}) and (\ref{Lumidef2}) one obtains

\begin{equation}
   h_{df} = \frac{24}{25}  \frac{R^{2}}{cr} \frac{\dot P}{P}\kappa,
\label{Ampdef4}
\end{equation}
and
\begin{equation}
   L_{GW_{df}} = - \frac{2^9 3^2 \pi^2 }{5^5} \frac{c}{G} R^{4}\left(\frac{\dot P}{P^2}\right)^2\kappa^2.
\label{Lumidef3}
\end{equation}

Therefore, it is not necessary to be concerned about $\phi$ in the calculations of the luminosity and amplitude of GWs. Different values of $\phi$ is only import in the calculation of $B_{s}$. Noticing, however, that $\phi$ and $B_{s}$ are not independent, as can be seen from Eq.~(\ref{CMs}).

Another point to note here is that the GW amplitude (Eq. (\ref{Ampdef4})) depends on the square of the radius. However, it is worth recalling that for compact stars, as WDs, the mass is related to the radius so that the more massive the star is, the smaller the radius will be. Thus, the amplitude implicitly depends on the mass $M$.

One could argue that rotation could be also important in the deformation of the star. In fact, rotation modifies the equatorial radius of the star, as a result the amplitude of the GWs is affected, since $h_{df} \propto R^2$. Thus, the higher the rotation velocity is, the greater is the radius.

Now, we are ready to calculate the GW amplitude and luminosity for SGRs/AXPs as massive fast-spinning WDs. The next section is devoted to this issue as well as the corresponding discussion of the results.

\section{Results and Discussions}
\label{sec:9}

Here we consider that SGRs/AXPs are fast-spinning and magnetized WDs which emit GWs due to the deformation caused by their own intense magnetic field. For this study, we use the magnetic field values inferred from the canonical pulsar model (see Eq. (\ref{CMs})), where it is considered that all the spindown luminosity of the star is converted to electromagnetic luminosity.

Thus, using Eq. (\ref{Lumidef2}), we calculate the GW luminosity for several SGRs/AXPs, considering these objects as a very massive WD of $M_{WD} = 1.4 M_{\odot }$ and radius $R_{WD} = 1.0 \times 10^{8}$ cm \citep{2013ApJ...762..117B}. We adopted $\kappa\simeq 10$, which is a conservative value that holds for an incompressible fluid star with a dipole magnetic field \citep[see, e.g.][]{1954ApJ...119..407F}. Similar values are obtained when relativistic models based on a polytropic EoS with dipole magnetic field are considered  \citep[see, e.g.][]{2000A&A...356..234K}. In fact, this parameter can take different values depending on the EoS and the geometry of the magnetic field \citep[see, e.g.][for a usefull discussion regarding this issue]{2006A&A...447....1R}.

The result of this calculation is presented in Table \ref{tabla:efici_def_SGR}, which also displays the ellipticity $\epsilon$, the spindown luminosity $L_{sd}$ ($ = 4\pi^2 I_3 f_{rot} \dot{f}_{rot} $) and the efficiency $\eta_ {df}$ ($=L_{GW_{df}}/L_{sd}$). Notice that the efficiencies are around $10^{-9}$ to $10^{-13}$. This implies that the gravitational luminosity is much smaller than the spindown luminosity when considering the magnetic fields inferred by the dipole model. Thus, we see that we can apply these magnetic field values to calculate the  GW amplitude, since the emission of gravitational energy is negligible as compared to the rotational energy loss rate, not changing significantly the inferred magnetic fields.

\begin{table*}
\begin{center}
\caption{ Parameters for SGRs/AXPs based on a very massive white dwarf of fiducial parameters, $M_{WD} = 1.4 M_{\odot }$ and radius $R_{WD} = 1.0 \times 10^{8}$ cm~\citep{2013ApJ...762..117B}. We adopt in the calculation $\kappa = 10$.}
\begin{tabular}{lccclc}
\hline
\multicolumn{6}{c}{\textbf{SGRs/AXPs  as massive WD of $M_{WD} = 1.4 M_{\odot }$}} \\ \hline
\textbf{SGRs/AXPs} & \begin{tabular}[c]{@{}c@{}}$B_{s}\sin{\phi}$ \\ ($10^{10}$ G)\end{tabular} & \begin{tabular}[c]{@{}c@{}}$\epsilon$\\ ($10^{-6}$)\end{tabular} & \begin{tabular}[c]{@{}c@{}}$L_{sd}$ \\ ($10^{37}$ erg/s)\end{tabular} & \multicolumn{1}{c}{\begin{tabular}[c]{@{}c@{}}$L_{GW_{df}}$ \\ (erg/s)\end{tabular}} & \begin{tabular}[c]{@{}c@{}}$\eta _{df}$\\ ($10^{-10}$)\end{tabular} \\ \hline
CXOU J010043.1-721134 & 4.12 & 3.28 & 1.59 & \multicolumn{1}{c}{5.48 $\times 10^{27}$} & 3.43 \\
4U 0142+61 & 1.41 & 0.382 & 0.135 & \multicolumn{1}{c}{4.59 $\times 10^{25}$} & 0.340 \\
SGR 0418+5729 & 0.0640 & 0.000790 & 0.000234 & \multicolumn{1}{c}{1.51 $\times 10^{20}$} & 0.000645 \\
SGR 0501+4516 & 1.96 & 0.745 & 1.36 & 2.05 $\times 10^{27}$ & 1.51 \\
SGR 0526-66 & 5.87 & 6.66 & 3.19 & 2.20 $\times 10^{28}$ & 6.91 \\
1E 1048.1-5937 & 4.05 & 3.16 & 3.66 & 1.87 $\times 10^{28}$ & 5.10 \\
1E 1547.0-5408 & 3.34 & 2.15 & 235.0 & 7.92 $\times 10^{30}$ & 33.7 \\
PSR J1622-4950 & 2.89 & 1.60 & 9.20 & 5.30 $\times 10^{28}$ & 5.75 \\
SGR 1627-41 & 2.36 & 1.07 & 47.7 & 5.11 $\times 10^{29}$ & 10.7 \\
CXOU J164710.2-455216 & 0.692 & 0.0924 & 0.0147 & 8.10 $\times 10^{23}$ & 0.0552 \\
1RXS J170849.0-400910 & 4.92 & 4.67 & 0.641 & 1.66 $\times 10^{27}$ & 2.59 \\
CXOU J171405.7-381031 & 5.25 & 5.33 & 50.1 & 1.23 $\times 10^{30}$ & 24.5 \\
SGR J1745-2900 & 2.43 & 1.14 & 11.4 & 6.18 $\times 10^{28}$ & 5.41 \\
SGR 1806-20 & 20.5 & 81.3 & 50.4 & 4.84 $\times 10^{30}$ & 96.0 \\
XTE J1810-197 & 2.20 & 0.937 & 2.00 & 4.11 $\times 10^{27}$ & 2.05 \\
Swift J1822.3-1606 & 0.141 & 0.00386 & 0.00153 & 5.58 $\times 10^{21}$ & 0.00365 \\
SGR 1833-0832 & 1.73 & 0.576 & 0.354 & 2.40 $\times 10^{26}$ & 0.677 \\
Swift J1834.9-0846 & 1.49 & 0.430 & 22.8 & 1.07 $\times 10^{29}$ & 4.70 \\
1E 1841-045 & 7.37 & 10.5 & 1.09 & 5.56 $\times 10^{27}$ & 5.08 \\
3XMM J185246.6+003317 & 0.427 & 0.0352 & 0.00397 & 7.05 $\times 10^{22}$ & 0.0177 \\
SGR 1900+14 & 7.34 & 10.4 & 28.7 & 7.43 $\times 10^{29}$ & 25.9 \\
SGR 1935+2154 & 2.29 & 1.01 & 18.3 & 1.18 $\times 10^{29}$ & 6.45 \\
1E 2259+586 & 0.617 & 0.0735 & 0.0624 & 6.34 $\times 10^{24}$ & 0.102 \\ \hline
\end{tabular}
\label{tabla:efici_def_SGR}
\vskip0.3cm

\end{center}
\end{table*}

It is worth recalling that the rotation periods as short as the ones observed in SGRs/AXPs, which ranges from, $P\sim 2-12$~s, can be really attained by WDs. \citet{2013ApJ...762..117B} showed that the range of minimum rotation periods of massive WDs is of $0.3\leq P\leq 2.2$~s, depending on the nuclear composition~\footnote{The relatively long minimum period of $^{56}$Fe spinning WDs,$\sim2.2$~s, implies that spinning WDs describing SGRs/AXPs have to be composed of nuclear compositions lighter than $^{56}$Fe, e.g., $^{12}$C or $^{16}$O~\citep[see][for details]{2013ApJ...762..117B}}. We refer the reader to the paper of these very authors for further discussion and details.

Figure \ref{fig:1} shows the GW amplitudes versus the magnetic fields for the 23 confirmed SGRs/AXPs (see also Table \ref{tabla:SGR/AXP}). Besides our fiducial WD model ($M_{WD} = 1.4 M_{\odot }$ of $R_{WD} = 1.0 \times 10^{8}$ cm), we consider two additional models, namely,
1.2 $M_{\odot }$ [$R_{WD} = 6.0 \times 10^{8}$ cm] and 1.0 $M_{\odot }$ [$R_{WD} = 7.5 \times 10^{8}$ cm] \citep[see][for further details about the mass-radius relation]{Boshkayev2013}. We stress that the stability of rotating WDs was analyzed taking into account the mass-shedding limit, inverse $\beta$-decay, and pycnonuclear instabilities \citep[see also][for several macro and micro instabilities in WDs]{2014ApJ...794...86C}, as well as the secular axisymmetric instability \citep[see Fig.1 of][for details]{Boshkayev2013}.
Note that for a given source the predicted magnetic field (GW amplitude) can vary almost two orders of magnitude depending on the assumed parameters.

\begin{figure}
\centering
\includegraphics[width=8.9cm, height= 6.5cm]{fig1.png}
\caption{GW amplitude as function of the magnetic field for SGRs/AXPs as fast-spinning and magnetized WDs.}
\label{fig:1}
\end{figure}

Figure \ref{fig:2} shows the GW amplitude as a function of frequency for some SGRs/AXPs, where the bullets stands for $M_{WD} = 1.2 M_{\odot }$ and the vertical bars, that crosses the bullets, stands for  $1.0 M_{\odot} \leq   M_{WD} \leq  1.4 M_{\odot} $, from top to bottom.
We also plot the sensitivity curves for BBO and DECIGO. It is worth mentioning that to plot the sensitivity curves, we use the minimum amplitude, $h_{min}$, that can be measured by the detector, for a periodic signal, for a given signal-to-noise ratio (SNR) and observation time $T$ \citep[see, e.g.,][for further details]{maggiore/2008}. Thereby, Fig. \ref{fig:2} presents the GW amplitudes for the sources ($h_{df}$) and the sensitivity curves are set to SNR = 8 and $T = 1$ year. Note that we do not display the sensitivity curve for LISA because these sources are far below it.

\begin{figure}
\centering
\includegraphics[width=9.2cm, height= 6.9cm]{fig2.png}
\caption{GW amplitude as a function of frequency for SGRs/AXPs as fast-spinning and magnetized WDs for masses in the interval  $1.0 M_{\odot} \leq  M_{WD} \leq  1.4 M_{\odot}$ (or $7.5 \times 10^{8}$ cm $\geq  R_{WD} \geq 1.0 \times 10^{8}$ cm), represented by the vertical bars, from top to bottom. The bullets stand for $M_{WD} = 1.2 M_{\odot }$ ($R_{WD} = 6.0 \times 10^{8}$ cm). Also plotted the sensitivity curves for BBO and DECIGO for $SNR = 8$ and integration time $T = 1$ year.}
\label{fig:2}
\end{figure}

Notice that some SGRs/AXPs produce GWs with amplitudes that can be detected by BBO and DECIGO. For example, 1E 1547.0-5408 and SGR 1806-20 could well be detected for the entire mass range considered. SGR 1900+14 and CXOU J171405.7-381031, in turn, are detectable for the entire mass range only by BBO. For these sources to be observed by DECIGO, they must have mass $M_{WD} \lesssim 1.3 M_{\odot }$. The sources Swift J1834.9-0846, SGR 1627-41, PSR J1622-4950, SGR J1745-2900 and SGR 1935+2154 could be observed by BBO and DECIGO if they have mass $M_{WD} \lesssim 1.3 M_{\odot }$ and $M_{WD} \lesssim 1.2 M_{\odot }$, respectively. However, if these SGRs/AXPs have $M_{WD} \sim 1.4 M_{\odot }$, they should be detectable only by BBO and with an integration time of $T = 5$ years. XTE J1810-197, SGR 0501+4516 and 1E 1048.1-5937 could also be seen by BBO and DECIGO if these objects have $M_{WD} \lesssim 1.3 M_{\odot }$ and $M_{WD} \lesssim 1.2 M_{\odot }$, respectively, but they will not be observed if they have mass $M_{WD} \sim 1.4 M_{\odot }$, even considering  $T = 5$ years.

Therefore, SGRs/AXPs described as WDs, which have moments of inertia four orders of magnitude greater than a NS, would generate GW amplitudes much larger than SGRs/AXPs described as NSs (see Figure \ref{fig:3}). Consequently, if these sources are NSs the GW amplitudes generated are far below the sensitivity curves of BBO and DECIGO. Thus, if these space based instruments observe continuous GWs from these SGRs/AXPs, this would corroborate the model of fast-spinning and magnetic WDs. This supports the description of SGR and AXPs as belonging to a class of very fast and magnetic massive WDs in perfect accord with recent astronomical observations of HMWDs.

\begin{figure}
\centering
\includegraphics[width=9.2cm, height= 6.7cm]{fig3.png}
\caption{ GW amplitude as a function of frequency for SGRs/AXPs as NSs. Also plotted the sensitivity curves for BBO and DECIGO for $SNR = 8$ and integration time of $T = 1$ year. We consider a NS of $M = 1.4 M_{\odot}$, radius $R = 10$ km and ellipticity given by  $\epsilon = 10 B^2 R^4 \sin^2{\phi} / G M^2$ from \citet{2017EPJC...77..350D}. }
\label{fig:3}
\end{figure}

It is worth noticing that from Eq. (\ref{Ampdef4}) that $h_{df} \propto \kappa$. Thus, if we consider an even more conservative value for $\kappa$, e.g., of the order of the unit, the GW amplitude decreases an order of magnitude and some sources in Fig. \ref{fig:2} will be below the sensitivity curves of BBO and DECIGO. XTE J1810-197, SGR 0501 4516 and 1E 1048.1-5937, for example, will be not detected with this $\kappa$ value, whereas the sources 1E 1547.0-5408 and SGR 1806-20 must have mass $M_{WD} \lesssim 1.3 M_{\odot }$ to be seen by the two spacial detectors. As for the other detectable sources in Fig. \ref{fig:2}, they cannot be too massive ($\gtrsim$ $1.2 M_{\odot }$) to continue being observed by BBO.

\section{Summary}
\label{sec:13}

Besides the search and detection of GWs from the merger events \citep{Abbott_2019,abbott2017d}, the search for continuous GWs has been of great interest in the  scientific community. It is well known that, besides compact binaries, rapidly rotating NSs are promising sources of GWs which could be detected in a near future by Advanced LIGO (aLIGO) and Advanced Virgo (AdV), and also by the planned Einstein Telescope (ET) and the space-based LISA, BBO and DECIGO. These sources generate continuous GWs whether they are not perfectly symmetric around their rotation axis, i.e. if they present some equatorial ellipticity. Undoubtedly, SGRs and AXPs are also good candidates in this context. Here we investigate the gravitational radiation from these objects described as fast-spinning WDs using the magnetic deformation mechanism. It is worth stressing that these putative uncommon WDs are known to have a high rotation (a few seconds to minutes) and a huge magnetic field ($10^{6}$ G to $\sim 10^{10}$ G).

Then, by describing SGRs/AXPs as rotation-powered WD pulsars, we consider the role played by the magnetic dipole field on the deformation of these objects and its consequences as regards the generation of GWs considering a mass range $1.0 M_{\odot} \leq   M_{WD} \leq  1.4 M_{\odot}$ for these sources. It is worth mentioning that, this is the first time in the literature that the GW counterpart for SGRs/AXPs are modeled as fast-spinning and magnetized WDs.

We note that some SGRs/AXPs, described as fast-spinning and massive WDs, emit GWs with amplitudes that could be detected by BBO and DECIGO, namely: 1E 1547.0-5408 and SGR 1806-20 can be observed for the entire considered mass range for one year of observation time, while SGR 1900+14, CXOU J171405.7-381031, Swift J1834.9-0846, SGR 1627-41, PSR J1622-4950, SGR J1745-2900 and SGR 1935+2154 can be detected for the entire considered mass range for five years of observation time. The sources XTE J1810-197, SGR 0501+4516 and 1E 1048.1-5937, in turn, can also be observed if they do not have so large masses.

Last but not least, it is worth mentioning that recent astronomical observations suggest that we should revisit the real nature of AXP/SGRs: are they really magnetars or fast-spinning and magnetized WDs? Thereby, a possible detection of continuous GWs coming from SGRs/AXPs would be a good indication that could corroborate the WD model, because for the NSs description, they are far below the BBO and DECIGO sensitivity curves.  We also encourage  future observational campaigns to determine the radii and the magnetic field of these sources to elucidate the real nature of SGRs and AXPs.

\section*{Acknowledgements}
We thank the anonymous referee for useful criticisms and suggestions which have improved our paper.
M.F.S. thanks CAPES for the financial support. J.G.C. is likewise grateful to the support of CNPq (421265/2018-3 and 305369/2018-0). J.C.N.A. thanks FAPESP (2013/26258-4) and CNPq (308367/2019-7) for partial financial support.

\section*{Data Availability}

The data underlying this article will be shared on reasonable request to the corresponding author.

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


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I knew, because of my frequent calls at Radek's office, that he was in daily consultation with Stalin. Sometimes he would dash over to Stalin's office several times a day. Every phrase he wrote was subject to Stalin's personal supervision. The articles were in every sense a joint labour of Radek and Stalin.
While these articles were in preparation, Commissar Litvinov was keeping on with efforts towards an agreement with Hitler. In April, he proposed to Germany a joint undertaking to preserve and guarantee the independence and inviolability of the Baltic States. Berlin rejected the proposal.
The Radek article was hailed widely as foreshadowing a Soviet turn towards France and the Little Entente, and away from Germany. " German Fascism and Japanese imperialism," wrote Radek, "are in a struggle for a redivision of the world-a struggle directed against the Soviet Union, against France, Poland, Czechoslovakia, Rumania and the Baltic states ; against China and the United States of America. And British imperialism would like to direct this struggle exclusively against the Soviet Union."
At this time I had quite a conversation with Radek. He knew that I was familiar with his assignment. I made some remark about our "new policy" and spoke of the impression it was creating in uninformed circles.
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Given the rustic tone of his music, it seems appropriate that Gregory Alan Isakov recorded his fourth full length record, Evening Machines, in his barn-turned-studio in Colorado. The album, released Oct. 5, blends a familiar palette of indie-folk tropes with elements of haunting electronic production.
The Tribune team sits down with the boys from Ivytide to hear a couple tracks off their new EP!
While late September is commonly known as midterm and rain season, for the past decade and a half, the start of fall has also been synonymous with POP Montreal. From Sept. 26-30, the annual festival took over the Mile End, pushing aside third-wave coffee venues and bicycle co-ops to make space for over 450 performers. With such a breadth of acts, the sheer selection can be overwhelming.While the A&E team couldn't decide on who deserved the crown, we still have the authority to bestow superlatives to our favourite acts.
For many students, it often feels impossible to pursue creative growth alongside academic demands—yet U3 McGill psychology student Vikki Gilmore is doing just that. The McGill Tribune sat down with the singer-songwriter to talk about her new EP, Someone, and the inspiration behind her work.


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Read Next Edward Norton Remembers 'Fight Club' Co-Star Meat Loaf: 'To Us He Will Always Be 'Bob''
Home Movies Movie News
July 22, 2017 2:31PM ET
John Heard, 'Home Alone' Actor, Dead at 72
Veteran of TV and film also delivered memorable roles in 'After Hours,' 'Big,' 'The Sopranos' and 'Cutter's Way'
John Heard, the actor who portrayed Kevin McAllister's father in a pair of 'Home Alone' films, has died at the age of 72.
Rodrigo Vaz/FilmMagic
John Heard, the actor who portrayed Kevin McCallister's father in a pair of Home Alone films, has died at the age of 72.
The Santa Clara Medical Examiner's office confirmed Heard's death, Variety reports. TMZ adds that the actor was found dead in his Palo Alto, California hotel room, just days after Heard underwent minor back surgery, his rep said.
An Obie Award-winning actor before he came to Hollywood, Heard broke out in the late Seventies thanks to his role in Chilly
Scenes of Winter, which was followed by starring roles in 1980's Heart Beat, where he portrayed Jack Kerouac, and 1981's Cutter's Way, with Heard delivering a remarkable turn as a conspiracy-minded Vietnam vet. Essentially ignored upon release, the film has since earned a reputation as a forgotten classic.
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John Heard- what a wonderful actor. We were in the movie Cutter's Way together & I got to experience his artistry and dedication first hand.
— Jeff Bridges (@TheJeffBridges) July 22, 2017
The early Eighties also found Heard in prominent roles in films like C.H.U.D., Cat People and Martin Scorsese's After Hours, where the actor played a seemingly sympathetic bartender. Toward the end of the decade, Heard found his niche giving depth to supporting roles, whether as Tom Hanks' nemesis in Big or Bette Midler's husband in Beaches.
Rosanna Arquette, who played Heard's girlfriend in After Hours (although they didn't appear on-screen together), wrote on Facebook, "Rest In Peace John Heard. Brilliant artist. My roommate in NYC .. in the 80s , my mentor in those years. Coach for Baby It's You. You always made me laugh ..heartbroken."
However, Heard will be most remembered as Macaulay Culkin's father Peter McCallister in the 1990 smash Home Alone and its 1992 sequel Home Alone 2: Lost in New York.
"At the time, we didn't know the movie was funny," Heard said of the role to Baltimore Media Blog. "We were playing the parents who lost their kid, so we didn't how funny-stupid we could be."
Thanks to the success of the film, Heard would be referred to on the street as "Home Alone Dad," even though the actor's résumé logged dozens of TV and film credits over the ensuing decades, including roles in My Fellow Americans, Awakenings, In the Line of Fire, Pelican Brief, Pollock, Sharknado and an Emmy-nominated reoccurring role as a duplicitous detective on The Sopranos. Most recently, Heard appeared on the Fox police drama APB, although the actor was set to appear in the film Last Rampage that's due out in September.
"I am shocked and saddened to awake to the news that John Heard passed away last night," actor Robert Patrick, who starred alongside Heard in Last Rampage, wrote on Instagram. "Such a gifted actor! I am so grateful I had the opportunity to watch, work, and spend time with him. This is tragic news."
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text:
Q: Other than heap size what would limit the number of elements a HashMap can hold As per the title - what constrains the number of elements a HashMap can hold and what data structure could be used instead.

A: The fact that hashCode returns an int instead of a long also prevents HashMap from being efficient much beyond 2^32 entries.

A: One thing is the maximum array size, which in Java is Integer.MAX_VALUE.
If that's a limit to you, then you could create your own class which wraps a list of HashMap objects or use a LinkedHashMap.

A: The only constraint would be array size (2^31-1) and the number of unique values possible for your key type.

A: I don't really think there are limitations.
Firstly, an object's hashCode will fit always in the maximum array size as the largest int value gives the maximum array size.
Secondly, afaik a HashMap uses lists for their keys. Therefore, if two keys have the same hashCode (which may happen even if you insert only some values) they will be inserted anyway. Since a list can get as long as you want there are no real limitations besides the efficiency of it.

A: The HashMap data structure is backed by an array for the hashtable under the hood.  Because Java array sizes must be specified using integers, they are limited in size to Integer.MAX_VALUE (about 2 billion elements).
If constant-time lookups of more elements are necessary, I suppose you could wrap nested HashMaps in your own class definition, but you're also going to have to get around the fact that Java's Collection interface specifies an int size value - in a nutshell, it's possible to have a data structure that stores more than Integer.MAX_VALUE elements, but this is not truly supported by anything in the Collection interface.

A: With the exception of the heap size that you've already mentioned I do not believe there are any hard limits on the number of items you can place into a HashMap.
Internally HashMaps have an array of 'buckets', with each bucket being a linked list. When you add an item it is hashed to find the correct bucket, and is then added to the front of that linked list. As such, even if every bucket has one item in it, adding one more item will simply add the item to the linked list in the bucket.
The behaviour I've described above is the implementation of the HashMap class that comes with the Oracle JRE and may differ on other platforms, and so other platforms may have limitations on the number of items that can be placed into them.
It is also worth pointing out that if you are putting more than Integer.MAX_VALUE items into a HashMap, the lookup performance will degrade considerably because the HashMap will have to iterate over the list when trying to find the item.

redpajama_set_name: RedPajamaStackExchange


The law ensures that Coos and Scoffs cannot claim they were not aware of financial problems and wrong doings. They are required to take individual responsibility that the financial records are being reported accurately. The law also require that audits are performed by external and independent auditors to avoid conflict of Interest. The firms used for audits cannot perform non-adult related work for the company. Auditing firms must also be rotated. 2. Employees that make the decision to whistle low are protected from retaliation from their employer.
They cannot be fired, 3. Tort reform in Texas currently only covers medical malpractice and caps damages that can be received at $250,000. This strips away the ability for a jury to decide the monetary amount to be paid. This cap also makes it more difficult for a victim to find a lawyer to even take their case, which often results in them never getting their day in court. Tort reform in Texas is saving money, but the beneficiaries of that savings are medical practitioners and insurance companies.
The lower cost of medical care for the citizens from this reform has not been shown. Insurance is lower for doctors now but that savings Is not being passed on to the patients, many of whom voted for tort reform for that reason alone. 4. Equal employment opportunity has Improved since the Call Rights Act of 1964. 5. Honesty Integrity – Doing what is right when no one is looking. Employees must make ethical decisions Transparency Fairness Respectful 6. Violation of intellectual property law can include copyright, trademark or trade secret infringement as well as patent damages.
In order for the general public to continue to benefit from the creation of new technology, art, music etc. The Inventors of IP must have confidence that their work Is protected and they will be able to benefit off of It. Along the Invention on new IP follows new Jobs as well. By protecting the rights of the owners of this property, we are also ensuring new jobs for the future. 7. Affirmative action should continue because the disparity is still too significant to ay things are now equal.
While we have certainly come a long way by opening doors that would have otherwise been closed; however, the difference is mostly seen on lower and some mid-level positions. It is argued that affirmative action is reverse discrimination for white men, but with 95% of senior level managers being men and 97% being white, but the static do not support this being true. An alternative to affirmative action would be to trust that companies will be fair and not discriminate; forever, as with other Issues companies mostly have a track record of doing the right thing when they are forced to.
BY -reel 579 are performed by external and independent auditors to avoid conflict of interest. The firms used for audits cannot perform non-audit related work for the company. Can be received at $250,000. This strips away the ability for a Jury to decide the monetary amount to be paid. This cap also makes it more difficult for a victim to find now but that savings is not being passed on to the patients, many of whom voted for rot reform for that reason alone. 4.


Solecare Podiatry is located on the first floor at Riccarton Clinic and can be accessed by lift and stairs. It is run by Mark Smith. Solecare Podiatry is ACC approved. Bookings are taken at Riccarton Clinic Reception 343 3661. Initial appointments are 40 minutes duration. Payments are made at the Riccarton Clinic reception desk.
Solecare Podiatry can advise on and provide treatment for a wide range of foot and ankle problems. From simple needs such as thickened toe nails, corns or a 'WOF' for the feet, through to complex problems of the foot and ankle, our team have the skills and experience to treat many common foot problems.
Solecare is ACC approved, but not all foot injuries qualify for ACC funding.


LEBANON, NH - Even a zap from a taser was reportedly not enough to convince a Plainfield man to call it a night and leave a bar late Saturday evening, Lebanon Police said in a release Monday.
Joshua Goodwin, 33, will be facing misdemeanor charges of criminal trespass, resisting arrest, simple assault on a police officer and disorderly conduct stemming from the incident that Lebanon Police said began around 11:20 p.m. on Saturday, July 8th when a local establishment called for help, saying that an intoxicated male was refusing their requests to leave the bar area of their restaurant.
Once police arrived, Goodwin "was repeatedly asked to leave by the officers and each time the intoxicated male subject refused," police recounted, continuing, "Officers then advised (Goodwin) that he was under arrest and attempted to take him into custody, at which time (Goodwin) began to physically resist. Officers utilized a Taser in an attempt to take (Goodwin) into custody, but (Goodwin) continued to resist and struggle with the officers."
Goodwin was eventually handcuffed and taken in for processing, after which he was released on $1,500 personal recognizance bail with a citation to be arraigned on September 11, 2017 at the Lebanon District Court.


AXIA Architects spent a day at Safari West to celebrate Karen Pregler's 23 years with AXIA. Karen will retire from AXIA Architects at the end of 2015. She spent the majority of her career with AXIA Architects and its predecessor firm, Witter Jefferies Architects, becoming a partner in 2001.
After graduating from Berkeley in 1976, Karen worked for various architectural firms including, MEA Group, Lawry Coker DeSliva Architects, and Robert Anderson. Karen landed at Witter Jeffries Architects in 1992, focusing on education projects. Her eleven year commitment to complete Ukiah High School Modernization was a highlight of her career.
Karen has served on the boards of the AIA and CSI local professional organizations.
Karen and husband Bill plan on traveling in 2016, with trips to Costa Rica and the Hudson River Valley. She is also looking forward to spending more time with her twin granddaughters, who live in the bay area. Karen will miss her wonderful AXIA family, but is looking forward to slowing down a bit to enjoy the next chapter in her life.
AXIA Architects will miss Karen immensely and look forward to seeing photos from her travels and life's adventures.


Pick brick for iconic exterior style.
Did you grow up dreaming of a classic brick house with a white picket fence? There's a reason bricks have remained such a popular home exterior material throughout the years that goes beyond just color and style.
In addition to great looks, brick also offers exceptional durability, protecting your home without the need for constant cleaning and maintenance. Brick homes are built to last, especially when you choose the professional contractors at Eagle Construction for your next brick remodeling project!
Why is brick better? Let us count the ways.
Brick siding offers excellent protection from the weather and other elements. Properly installed brick is long lasting, so you'll save money on replacements and repairs.
Exterior brick will never go out of style. You'll have a look you'll love for years and, if you ever decide to sell, you'll see an impressive return on investment.
Outside brick doesn't need to be cleaned as frequently as other types of siding, so when warm weather comes you'll have extra time to focus on what's really important.
Choose and combine brick types to add a personal touch.
Choose whatever type you like, or let us guide you to the right decision for your layout and location. Some brick can even be painted for even more customization.
We know that home improvements can be expensive, and as homeowner you want to make sure you're getting the most out of the money you spend. That's why we only use the best materials sourced from local suppliers, so you can have the quality you deserve at a surprisingly affordable price.
If you're interested in seeing what Eagle can do for you, check out our portfolio page for inspiration. In addition to brick repair, installation and replacement, we offer a full range of exterior and interior remodeling services.
With our years of experience and dedication to our craft, Eagle Construction is the best choice for exterior remodeling in the local area. If you want to know more about beautiful, durable outside brick and how it can benefit your home, don't hesitate to schedule a consultation!
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Addressing the UN: Par for the Course (work)
For the past several years, Pace University's International Disarmament Institute, the Political Science Department, and the Peace and Justice Studies program have collaborated to craft a joint statement on youth engagement and disarmament education to deliver to the...
Building on the Legacy of the Society of Fellows
Under new leadership, the Society of Fellows is eyeing the future and building on four decades of scholarly excellence. In her first year as chair of the Society of Fellows, Judi Pajo, PhD, is focused on honoring tradition and embracing innovation. For four decades,...
$513,171 Total amount of continued and new funding for 21-22 Mancini Receives NIH Grant to Study COVID-19 Impacts Associate Professor of Psychology, Anthony Mancini, PhD, received a four-year, $440,632 grant from the National Institutes of Health (NIH), which took...
Dyson faculty have been sought out to share their research and expertise, providing insightful quotes for major news outlets. Clinical Associate Professor of Economics Mark Weinstock, CBE Quoted on News12, June 2022 On proposed Federal Reserve interest rate hikes as...
All About the Environment
Professor Rubbo, Students Conduct Environmental Studies for Connecticut Town Students in ENV 498, a research practicum taught by Michael Rubbo, PhD, clinical associate professor of environmental science, spent the spring semester conducting biodiversity studies for...
Watching the Waterways: The PaceDocs Production of Tide to Table On May 10, 2022, the Media, Communications, and Visual Arts department's award-winning documentary film team—PaceDocs—premiered Tide to Table: The Remarkable Journey of Oysters, which focuses on the...
Lessons in Legislative Action
Dyson College Institute for Sustainability and the Environment Lessons in Legislative Action Working with New York State lawmakers, Pace environmental clinic students have successfully initiated new legislation to reduce pollution from road salt. W hile sodium...
The New Face of Trauma
The New Face of Trauma Groundbreaking research indicates there could be a positive side to negative events. Can anything positive possibly come from an adverse event such as a flood, a mass shooting, or a catastrophic accident? The answer is yes, according to trauma...
Rewarding Research
Madison Ames '21, chemistry, is one of several outstanding Dyson students to receive recognition and support for her research. Showstoppers Dyson College research teams won the top prize at the annual Student-Faculty Research Showcases celebrating collaborative...
Humanities Goes High Tech
HUMANITIES Goes High Tech With new initiatives and pioneering instruction, Dyson College is poised to become a leader in educating students through the evolving arena of digital humanities. This is definitely not your parents' classroom. Today's students of language,...
Expanding Opportunitas
Expanding Opportunitas Two new PhD programs and a new bachelor's degree will provide increased options for the next generation of students and professionals. When, on October 8, 1974, the Dyson College of Arts and Sciences was officially named after Pace alumnus...
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Dean's Message: Dyson College's Legacy
Fed Challenge Team: Going Way Beyond the Numbers
CCAR: Changing Lives for 25 Years and Counting
Connecting Threads: History Summit
Dyson Alumni
Dyson Students Shine as Millennium Fellows
In the Field: Internships through the Wilson Center


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Home | Macro Markets update
Macro Markets update
US government bonds rates are close to their all-time lows (10-year rate in the 0.6% area), whereas German bond rates have been stabilising at around -0.4%
Carla Solera
Investor Relation Specialist
The below report is going to present the current Macro Markets update, which was prepared by Eurizon Asset Management.
Risk assets scored significant gains in the past month, making up in part the major losses incurred in the previous month. The recovery of risk assets materialized in an environment of easing volatility and was supported by a combination of good news on the containment of Coronavirus at the global level, and very determined economic policy actions aimed at containing the negative effects of the shutdown of the economies. Until lockdown conditions remain in place in the major economies, the combination of the slowdown of the contagion, and the economic policy responses, should allow investors to keep affording only secondary importance to economic data, that will increasingly outline a very sharp slowdown of the economy. However, starting from the second half of May, and in June, when social distancing measures will be eased, focus will shift to the effects of the resumption of activity.
Risk assets scored significant gains in the past month, making up in part the major losses incurred in the previous month. Stock indices returned to levels roughly halfway between the highs hit in February and the lows marked in March. Spread bonds (Investment Grade, High Yield, Emerging markets) narrowed spreads, although the distance from the levels reached before the correction remains very substantial. US government bonds rates are close to their all-time lows (10-year rate in the 0.6% area), whereas German bond rates have been stabilising at around -0.4% for over a month. Spreads widened significantly on peripheral Eurozone government bonds, in waiting for more coordinated fiscal policy response at the European level.
The recovery of risk assets materialized in an environment of easing volatility and was supported by a combination of good news on the containment of Coronavirus at the global level, and very determined economic policy actions aimed at containing the negative effects of the shutdown of the economies. For what concerns the virus, evidence of a slowdown of the contagion in Italy since the end of March offered reassurances on the effectiveness of the social distancing measures adopted, fuelling positive expectations on containment in the other countries affected. More recently, further encouragement came from the fact that the contagion peak at the global level, and in the United States in particular, seems to become a couple of weeks before it was expected.
For what concerns economic policy measures, the US approach emerged as being the swiftest and most effective. The Fed, which had shown no hesitation in cutting rates to zero already in mid-March, then resumed QE, extending the range of assets eligible for purchase, to include Investment Grade bonds that, in the meantime, were at risk of being downgraded to High Yield status. A similar measure has been taken recently by the ECB, which will accept as collateral bonds subject to a rating downgrade to High Yield.
Fiscal Front
On the fiscal front, action was taken very swiftly and effectively in the United States, where Congress has already approved measures worth in excess of 2,000 billion dollars (12% of GDP). In the Eurozone, the Stability Pact has been suspended, allowing individual countries to put in place the necessary fiscal measures, straying from the budgetary frameworks approved by the EU Commission. As regards joint initiatives, the European Union has established a fund to protect jobs, enhanced the scope of action of the EBI, and offered unconditional credit lines for healthcare spending under the European Stability Mechanism (ESM): important actions, albeit not as fast and effective as taken in the US and, most importantly, lacking any major progress towards a more federalist approach that the issue of shared debt would have marked. The debate on this latter front is still open.
Until lockdown conditions remain in place in the major economies, the combination of the slowdown of the contagion, and the economic policy responses, should allow investors to keep affording only secondary importance to economic data, that will increasingly outline a very sharp slowdown of the economy.
However, starting from the second half of May, and in June, when social distancing measures will be eased, focus will shift to the effects of the resumption of activity. On this front, the spotlight will be on two main aspects. Firstly, the actual extent of the recovery of economic activity, that will depend heavily on which social distancing measures will have to stay in place. Secondly, the risk of the appearance of new contagion clusters following the easing of containment measures.
Market evolution
As regards the evolution of the markets, we note that even after the recovery scored in the past month, risk asset valuations still hold appeal, both in absolute terms, and in particular compared to the return offered by high-quality government bonds. US rates at 0.6% on the 10-year segment, and German Bond rates at -0.4%, are already pricing in ultra-conservative economic cycle scenarios. Investment Grade and High Yield bond spreads widened less than they did
during the 2008 crisis, which was a pure debt crisis (as is not the case today) and lacked the direct (Investment Grade) and indirect (High Yield) support provided by the central banks. Following the recent widening, these assets hold appeal. In a medium-term perspective, emerging country bonds also seem appealing, with spreads just below the highs hit in 2008,
although in this case no protection is offered by central banks (Fed and ECB), and low oil prices could keep volatility high on oil producer issues.
Peripheral Euro area
Peripheral Euro area bond spreads seem appealing, considering the ECB's approach, which seems set on containing financial tensions. It should be said that the major issues of debt that countries will have to face in the next few months could hinder a swift tightening of spreads. Lastly, stocks: valuations in absolute terms (price-earnings ratio, P/E) have returned to levels in line with long-term averages on most indices but are showing a smaller discount than they were following the 2008 correction. However, the sharp decline of interest rates makes return from corporate earnings, while uncertain and on the decline in the current economic picture, appealing in a medium-long term perspective.
The favorable indications on the containment of the contagion and the size of the economic policy measures put in place at the global level, advise taking a moderately pro-cyclical approach, with a few exceptions.
The investment view for Eurizon portfolios is neutral on US duration, negative on German and quasi-core Euro area government bonds. Overweighting confirmed of non-core Euro area government bonds. Overweighting view taken on the spread markets; the stepping up of positions, initiated already in the course of April, is mostly concentrated on the components supported by central banks, therefore Investment Grade bonds and, secondly, High Yield bonds. Neutral view confirmed on equity. The near terms outlook still seems uncertain, and the market will unlikely build on the rebound seen over the past few weeks; in any case, a flexible management approach will be maintained, considering potential corrections with an eye to gradually stepping up positions.
Asset Class View Commentary
Equity Neutral Neutral view confirmed on equity.
The near-term scenario still seems uncertain
and we believe
the market is unlikely to build on the rebound
seen over the past few weeks; in any case,
a flexible management approach will be
maintained, considering potential
corrections with an eye to gradually
stepping up positions.
bonds Neutral
Positive Neutral view on US duration, negative on Germany
and quasi-core Euro bonds.
Neutral view confirmed on US duration.
Negative view taken on German and
quasi-core Euro area government bonds,
confirming the portfolio adjustments made in the
the course of the month. Positive view on
peripheral Euro-area government bonds.
Overweighting confirmed of non-core Euro area
government bonds.
Spread bonds Positive Positive view on spread bonds.
Overweighting position taken on the spread
markets; the stepping up of positions, already
initiated in the course of April, was mostly
focused on the components supported by the
central banks, namely Investment Grade
bonds and, secondly, High Yield bonds.
Currencies Positive Yen Positive view on yen.
Positive view taken on the yen, confirming
the portfolio adjustments made in April.
Fixed Income, Insights
When bad news is good news
Andrew Lake, Head of Fixed Income at Mirabaud Asset Management, details his views on the fixed income markets and his outlook for 2023.
Equities, Insights
European fund flows 2022: contrasts and turning points
2022 was far more heterogeneous in active versus passive, asset manager and fund category flows than widely assumed.
Insights, Market Outlook
Why private market allocation should be higher?
According to PM Alpha wealth managers should consider a significant re-balancing of portfolios on behalf of clients.


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Thousands Descend On Staples For Monday Morning Kobe Bryant Memorial
Filed Under:Kobe Bryant, Kobe Bryant Memorial, Los Angeles Lakers, Remembering Kobe Bryant, Staples Center
HOW TO WATCH THE CEREMONY
LOS ANGELES (CBSLA) – Final preparations are underway Monday morning as Los Angeles prepares to say goodbye to Lakers legend Kobe Bryant.
Feb. 24, 2020. (CBS2)
With 90 minutes to go before the Celebration of Life ceremony, the security team at L.A. Live had set up fencing to prepare for the 20,000 people who will gather at 10 a.m. Monday at Staples Center to honor Kobe and Gianna Bryant, as well as the seven other victims of the Jan. 26 helicopter crash.
By 8 a.m., thousands of fans had already lined up outside.
Staples Center is expected to be busy Monday. It hosted a Kings game Sunday morning and a Lakers game earlier Sunday afternoon. It will also host a Clippers game Monday night.
More than 100,000 people tried to get tickets to the memorial. On Friday, officials reminded fans without tickets to avoid the area tomorrow.
"We hope that everybody heeds the message and they stay either in their offices, surrounded by their friends or at home with their family or loved ones, because it's going to be a very emotional memorial for that day and we want people to be able to enjoy it," Staples Center President Lee Zeidman told reporters outside the venue.
Line of ticket-holders waiting to pay tribute during today's public #KobeFarewell at #StaplesCenter @CBSLA pic.twitter.com/bjnJSewcrE
— Kara Finnstrom (@KaraFinnstrom) February 24, 2020
Zeidman was joined by Los Angeles Police Department Chief Michel Moore again to emphasize that the ceremony will not be broadcast on any of the outdoor screens at Staples Center or in the adjacent L.A. Live plaza. No restaurants at L.A. Live will be open during the ceremony.
Pico and Olympic boulevards and other major streets near the arena will remain open, but smaller streets outside Staples Center and L.A. Live will be blocked off and accessible only to people with tickets.
"This is, to be clear, a ticketed worldwide event at this location," Moore said. "And what that means is, if you don't have tickets and credentials, you will not be allowed into this venue. The point there is, do not impact the rest of the Los Angeles downtown community by trying to come here and be part of something that you'll not be a part of."
There is no indication that people will try to cause a disturbance, Moore said, adding the community has shown the utmost respect in the weeks following the Jan. 26 helicopter crash that killed Bryant, 41, Gianna, 13, and seven other people.
Zeidman didn't offer any details about how many tickets were purchased by fans, but 20,000 seats were made available in the arena for Monday's ceremony, which will start at 10 a.m. Doors to Staples Center opened at 8 a.m., and everyone with tickets is asked to be in their seats by 9:45 a.m.
There was no information on who will be speaking at the memorial.
Patrick Vuong and his girlfriend, Kelly Sadamitsu attended Sunday's Kings game in their Kobe jerseys.
"In the wake of Kobe's passing, I always feel like I should be honoring Kobe in some way," Vuong said.
They attended the hockey game with Sadamitsu's parents, who she said raised her on a well-balanced diet of L.A. sports.
"Just growing up, my parents watch the Lakers almost every game and it's something that help bring the family together," Sadamitsu said.
The ability to bond through grief is being felt by Jacqueline Rocha – who only learned this morning she was able to buy a pair of tickets for the memorial.
"I'm still in disbelief," Rocha said, "but I feel extremely lucky and blessed."
Kiara Arvizu is still on waitlist after driving 16 hours with her friends from Denver. She said Kobe's Mamba mentality is why they're not ready to give up.
"Like he always said, who cares if you shot and he missed. Keep trying. Same thing in this situation," Arvizu said.
Vuong will not be at the memorial but a piece of him will through his aunt and uncle who got tickets.
"They're very excited," he said. "My aunt is going try to borrow this jersey to wear tomorrow."


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The parking program has an administrative appeals process for individuals who believe that their parking citation was issued in error. The appeals process was authorized by the Town of Wrightsville Beach.
Any person who has received a parking citation has the right to file an Appeal. An Appeal form must be filed within 3 days of the citation issue date. Failure to submit an Appeal within the 3 day period will result in the relinquishment of your right to file an Appeal. While a citation is in the Appeals Process, the originally stated fine will not continue to escalate. Do not attempt to pay while your citation is under appeal. No refunds will be issued. All Appeals will be read and reviewed by the Appeals Committee, and a decision shall be made within 3-5 business days after being submitted.
The customer shall receive a phone call at the contact number provided on the Appeal Form informing them that their Appeal has been accepted. The citation will be voided in the system, and then no further action is necessary.
Any fines incurred by this point shall be waived.
The customer shall receive a letter in the mail at the address provided on the Appeal Form, informing them that their Appeal has been denied and that further action will need to be taken.
Following six days after the Denial Letter has been received (based on the date of postmark) and if no action has been taken to pay the citation, the fine will continue to increase as stated on the original citation.
When can my car be booted?
Who operates the parking program?


I want to know what the normal heart rate ?
I'm filling in a questionaire and i need to know what my maximum heart rate is and my resting heart rate but i don't even know what the normal heart is! i need to find out the normal heart rate to work out my maximum heart rate and resting heart rate.
Dear Chris, In answer to your medical question, the normal heart rate is 72 beats per minute. I therefore trust that this answers your medical question.
What causes rapid heart rate?
Last night, I woke up and I got thirsty but I had water right next to me since I m always thirsty so I drank some of it but then my heart started beating so fast for no reason. This has never happened before so I wanted to know if this is normal and I m just over reacting.
Is it normal to have a resting heart rate of 115 bpm?
Is a resting heart rate of 115 bad? And also, my wife and I went to an e.r. a few days ago because she had some bad stomach pain and she is pregnant and these doctors wanted to prep her for surgery for her appendix without knowing for sure that was what was wrong with her, is that typical procedure?


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Get Fundraising Support
Buy our Guide to Fundraising
Find Funds
Green Hall Foundation
Health & Social Care Older People
The Green Hall Foundation's aim is to sustainably improve lives among: the sick, the elderly, the disabled and the disadvantaged particularly in the UK. Overseas project are also supported provided that the applicant charity is registered in the UK.
Preference is given to appeals where the Foundation can meet a significant proportion of the funding required and to appeals where permanent equipment or building is required as opposed to funding salaries or the charity running costs.
Grants are typically between £1,000 – £10,000 with preference being given to funding specific projects or items of equipment. Only UK registered charities can apply. Running costs and salaries are not funded.
Deadline: Continuous rolling programme. The Trustees meet in May and November.
Each May meeting will be open to Charities in all income brackets.
Each November meeting will only be open to Charities with an annual income of £250,000 or less.
For more information and how to apply please click here.
Funds Closing Soon
Education & Employment Environmental Health & Social Care
Tuesday January 19th, 2021 11:59pm Education & Employment Health & Social Care
Dove: The CROWN UK Fund
Thursday January 21st, 2021 5:00pm Arts & Culture Covid 19
Department for Digital, Culture, Media & Sport: Culture Recovery Fund (Second Round)
Tuesday January 26th, 2021 12:00pm Covid 19 Heritage
Department for Digital, Culture, Media & Sport: Culture Recovery Fund for Heritage (Second Round)
Tuesday January 26th, 2021 2:00pm
Other Older People Funds
Covid 19 Older People
Persimmon Community Champions
Persimmon, UK house builders, Community Champions' funding programme is awarding grants of up £1,000 to community groups and charities that support the over-70s – a vulnerable group in our society that they feel need their support at this time of crisis. Deadline: Continuous rolling programme. For more information and how to apply please click here.
Read More Education & Employment Health & Social Care Older People Youth
Kent Community Foundation: Themed Funds
Kent Community Foundation's Themed Fund programme awards grants of up to £5,000 (£7,500 considered for exceptional applications) to not-for-profit organisations and registered charities with projects in one of the following themed areas: Employment, Skills & EnterpriseProjects which raise the aspirations and increase the skills and opportunities of people who are far from the labour market…
Read More Community Buildings/Halls Health & Social Care Older People Sports Youth
Burg-Wächter: Secure Communities Scheme
BURG-WÄCHTER, Europe's largest safe and post box manufacturer, is awarding up to £1,000 and security products/advice to charities, social enterprise, not for profit and community ventures to help secure their success. Any grassroots project or activity that would benefit most from this scheme are those with a security aspect as well as a funding need.…
Read More Health & Social Care Older People
Masonic Charitable Foundation: Later Life Inclusion Grant
The Masonic Charitable Foundation's Later Life Inclusion Grant awards grants of up to £80,000 to local and national registered charities that support disadvantaged and vulnerable older people over 50 years. Grants can be offered to charities that provide: Mental and physical health support Gateway and access to service, e.g. transport and technology Community based approaches, i.e. volunteering,…
Funding for All provides free, expert advice to the Kent and Medway voluntary sector. We can help secure your organisation's future by developing your skills in all aspects of fundraising.
Copyright © 2021 Funding for All. Registered Charity No. 1150204. Registered Company No. 08263265


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Corona Protection
Alcohol Wet Wipes
US Video Sport Business Simply Had Its Finest Could Since 2008; Prime 20 Finest-Promoting Video games Introduced
by SubSellKaro June 15, 2020 Gaming News
With more and more people staying home during COVID-19 lockdowns, spending on video games is jumping to heights not seen in more than a decade. The NPD Group has released its report for US video game industry sales in May, and they were huge.
Total spending on video games in the US during May 2020–covering hardware, games, and accessories–reached $977 million. That is up 52 percent compared to May 2019. According to the NPD, May 2020's $977 million was the highest for a May month since May 2008 ($1.2 billion).
Year-to-date, total spending on video games in 2020 reached $5.5 billion, which is up 18 percent. This represented the highest year-to-date spending since 2011 ($5.7 billion).
Software sales specifically reached $438 million for May 2020, which is up 67 percent year-over-year, and it's the highest since May 2010 ($487 million).
Call of Duty: Modern Warfare was the No. 1 best-selling game of May 2020. The game remains the top-selling game of 2020 to date, and the highest-selling game for the 12-month period ended May 2020. Rockstar's endlessly popular Grand Theft Auto V, which was just announced for PS5 and Xbox Series X, jumped up the charts to land at No. 2 for May 2020. Animal Crossing: New Horizons, NBA 2K20, and Mortal Kombat 11 rounded up the top five best-sellers for May 2020.
You can see the full Top 20 sales chart below. The report includes physical and digital sales, except for Nintendo's digital sales and titles sold on the Eshop.
None of May 2020's new releases made it into the top 10. Xenoblade Chronicles: Definitive Edition was the highest-ranking new release, coming in at No. 14. But since this is a Switch exclusive, its actual sales total was likely higher.
Moving to hardware, total spending rose 56 percent to $235 million. May 2020's numbers were the best for a May month since May 2010 ($239 million). The Nintendo Switch was the highest-selling home console of May 2020 in terms of both dollar and unit sales.
The Nintendo Switch's unit sales in May 2020 were the highest for a single platform during a May month since May 2009, when the Nintendo DS led the way.
Spending on accessories and game cards for May 2020 reached $304 million, which was up 32 percent. Microsoft's Xbox Elite Series 2 controller was the best-selling accessory of May 2020 and for the year to date.
The video game industry–in the US and globally–is expected to see a jolt in sales later this year when the PS5 and Xbox Series X launch this holiday season.
Top 20 Best-Selling Games Of May 2020 (US Only):Call of Duty: Modern WarfareGrand Theft Auto VAnimal Crossing: New Horizons*NBA 2K20Mortal Kombat 11Red Dead Redemption IIMinecraft*Final Fantasy VII: RemakeAssassin's Creed: OdysseyStar Wars Jedi: Fallen OrderMadden NFL 20Mario Kart 8 Deluxe*Need for Speed HeatXenoblade Chronicles: Definitive Edition*Minecraft Dungeons*Saints Row: The Third RemasteredMLB The Show 20Super Smash Bros. Ultimate*Call of Duty: Black Ops IIIFIFA 20
*Digital sales on Nintendo Eshop not included
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Meet the Mantra: A Streamlined Jet Ski from...
Meet the Mantra: A Streamlined Jet Ski from the Future
An ambitious team of boating experts has created a futuristic looking winged watercraft designed to race across open waters as incredible speeds.
Dubbed the Mantra, the streamlined vessel was entirely handmade and is decked out in striking black paintwork that helps make it look like something from a Star Wars movie.
It is the brainchild of an international team under the banner of Trydent Boats, which includes a race boat expert from the Philippines, an Australian entrepreneur, and an Italian mechanical engineer who has previously designed components for Ducati
According to its makers, the aesthetics of the Mantra were inspired by vintage cars and Filipino racing boats "Bancarera."
Furthermore, its trimaran wings have been designed to provide hydrodynamic lift at high speeds, along with making the craft extremely stable, which not only makes it easy to ride but also tons of fun.
As for performance, the Mantra can hit a top speed of 50mph and is also capable of "drift"-style cornering. It is powered by Honda's GX390 Mega Marine engine which can be activated by pressing a "start" button on the retro-styled instrument console.
The Trydent Mantra will be available to order soon through IndieGOGO, with an early-bird pricing of around $2,500.
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