text:
package sigar_test

import (
	. "github.com/onsi/ginkgo"
	. "github.com/onsi/gomega"

	"testing"
)

func TestStats(t *testing.T) {
	RegisterFailHandler(Fail)
	RunSpecs(t, "Sigar Suite")
}

redpajama_set_name: RedPajamaGithub


text:
Biografia

Nati a San Marino, Carlo Simoncini si trasferì con la famiglia a Trieste, dove lavorò nella marina mercantile astroungarica, mentre Sady Serafini si trasferì a Torino, dove lavorò come contabile.

Con l'inizio della prima guerra mondiale ritornarono a San Marino e risposero all'appello di Giuliano Gozi del 4 giugno 1915 per arruolarsi nel Regio Esercito.
Carlo venne iscritto come volontario a Forlì ed entrò nel 3º reggimento di artiglieria di montagna, mentre Sady venne iscritto come volontario a Rimini ed entrò nel 1º reggimento di artiglieria di Rimini, entrambi acquartierati presso la caserma D'Azeglio di Bologna prima di partire per il fronte sull'Isonzo.

Carlo sfuggì ad una granata shrapnel e raccolse la culatta, che inviò in Repubblica, ma il 9 luglio a Lucinico nei pressi di Gorizia, mentre era intento a posizionare un cannone, morì per lo scoppio di una granata e venne sepolto nel cimitero di Mossa.

Sady morì ad ottobre a causa delle ferite riportate in combattimento e venne sepolto nel cimitero di Gorizia.

Commemorazioni postume
Carlo Simoncini è immortalato come un bambino in fasce nella tempera di Emilio Retrosi nella sala del Consiglio Grande e Generale del Palazzo Pubblico e venne decorato con la Medaglia d'argento al valore militare.

I due sammarinesi furono ricordati con il discorso "Olocausto sammarinese" a Trieste il 19 dicembre 1918 dal futuro Capitano Reggente del Partito Fascista Sammarinese Manlio Gozi.

Nell'ottobre del 1925 le due salme tornarono a San Marino e, dopo una solenne cerimonia, furono deposte nella cappella di San Pietro, vicino alla Basilica, dove rimasero esposte per una settimana.

Il 13 ottobre 1927 il Consiglio Grande e Generale decorò entrambi con la Medaglia d'oro di 1ª classe al valore e il 29 ottobre venne inaugurata l'Ara dei Volontari alla presenza dell'onorevole Giovanni Giuriati in rappresentanza del governo italiano e dei Capitani Reggenti Gino Gozi e Marino Morri. Sull'Ara sono incisi i loro nomi.

Il 29 settembre 1929 venne inaugurata con una cerimonia ufficiale la loro tomba monumentale, disegnata dal romano Vincenzo Maraldi, al cimitero di Montalbo a Città di San Marino.

Il 6 luglio 2016 si è svolta una cerimonia ufficiale presso le loro tombe.

Onorificenze

A entrambi

Carlo Simoncini

Note

Bibliografia
Ten. Col. Sebastiano Ciacci, Discorso in occasione del centenario del supremo sacrificio del Caporale Carlo Simoncini e del Caporale Sady Serafini, San Marino, 6 luglio 2016.

Voci correlate
Giuliano Gozi
Prima guerra mondiale
Irredentismo italiano
Ara dei Volontari

Collegamenti esterni
San Marino. Centenario supremo sacrificio Caporale Carlo Simoncini e Caporale Sady Serafini

Irredentismo italiano
Sottufficiali e graduati del Regio Esercito
Medaglie d'argento al valor militare
Storia di San Marino
Morti a Gorizia
Coppie di persone
Persone della prima guerra mondiale

redpajama_set_name: RedPajamaWikipedia


text:
New paper finds another non-hockey-stick in the Atlantic Ocean
A paper published today in The Holocene finds another non-hockey-stick from reconstructed sea surface temperatures in the NE Atlantic and Nordic Seas over the past millennium. Plot of the data from the paper shows sea surface temperatures were higher during the Medieval Warming Period 1000 years ago than at the end of the record in 1975.
Plot of the data from the paper shows sea surface temperatures were higher during the Medieval Warming Period 1000 years ago that at the end of the record in 1975. Note vertical axis is inverted because the proxy is inversely related to sea surface temperature.
Update: Multiproxy data from the source noted in comment below also shows warmer temperatures during the Medieval Warming Period than at the end of the record in 1975:
Prior posts on non-hockey-sticks
Reconstructions of surface ocean conditions from the northeast Atlantic and Nordic seas during the last millennium
Laura K Cunningham et al
We undertake the first comprehensive effort to integrate North Atlantic marine climate records for the last millennium, highlighting some key components common within this system at a range of temporal and spatial scales. In such an approach, careful consideration needs to be given to the complexities inherent to the marine system. Composites therefore need to be hydrographically constrained and sensitive to both surface water mass variability and three-dimensional ocean dynamics. This study focuses on the northeast (NE) North Atlantic Ocean, particularly sites influenced by the North Atlantic Current. A composite plus regression approach is used to create an inter-regional NE North Atlantic reconstruction of sea surface temperature (SST) for the last 1000 years. We highlight the loss of spatial information associated with large-scale composite reconstructions of the marine environment. Regional reconstructions of SSTs off the Norwegian and Icelandic margins are presented, along with a larger-scale reconstruction spanning the NE North Atlantic. The latter indicates that the 'Medieval Climate Anomaly' warming was most pronounced before AD 1200, with a long-term cooling trend apparent after AD 1250. This trend persisted until the early 20th century, while in recent decades temperatures have been similar to those inferred for the 'Medieval Climate Anomaly'. The reconstructions are consistent with other independent records of sea-surface and surface air temperatures from the region, indicating that they are adequately capturing the climate dynamics of the last millennium. Consequently, this method could potentially be used to develop large-scale reconstructions of SSTs for other hydrographically constrained regions.
Posted by MS at 10:39 AM
I think the data series to use is:
ftp://ftp.ncdc.noaa.gov/pub/data/paleo/paleocean/by_contributor/cunningham2013/cunningham2013-data-series.txt
NENA_Comp column
MS June 18, 2013 at 1:10 PM
NENA_Comp column plotted in Update above
Just when the UK Met Office and warmists declare that :
http://www.bbc.co.uk/news/science-environment-22959578
MS February 4, 2014 at 11:13 AM
http://www.co2science.org/articles/V17/N6/C1.php
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redpajama_set_name: RedPajamaCommonCrawl


text:
Skyword Announces Skyword360, Powering a Content-Centric Approach to Extraordinary Customer Experiences
Company Also Announces Software Certification Program Through Skyword University
Boston, MA, June 14, 2018 – Skyword, the leading content marketing software and services company, announced Skyword360, the next generation of its content marketing platform, at their Forward 2018 conference. The newly redesigned platform now includes end-to-end capabilities to manage and execute content strategies and operations across the entire enterprise.
Now with enterprise-wide visibility and planning functionality, Skyword360 enables marketing leaders and teams to coordinate content strategies across multiple audiences, campaigns, channels, divisions, and regions. With this unified approach, enterprises can create unique customer experiences that differentiate their brand and drive measurable results.
"Today, CMOs know they can't harass their customers into buying from them. Instead brands must create experiences that their customers want or need. And to do this, they need to create content-brilliantly, consistently, and everywhere their customers want to spend their time," said Tom Gerace, CEO of Skyword.
"But most companies lack the operational model and infrastructure to make this effective," Gerace continued. "We've reimagined the Skyword Platform and created Skyword360 to power a unified content-centric model for creating exceptional customer experiences."
Skyword360 Certification
Skyword also announced its newly launched certification program through which customers can become Skyword360 Champions as part of Skyword University's training and education initiatives. To ensure marketers' success, Skyword has developed a certification program where they can ensure that their teams have mastered the technology through a series of training modules and tests. Skyword customers can use this to train existing team members and, when they need to hire for their content teams, recruit Skyword Champions to their organizations.
Overview of Platform
The new platform includes a redesigned user interface to easily navigate from an enterprise view of content strategy to more in-depth views of individual channels.
Key elements of the platform include:
Strategize
Within Skyword360 marketers can document their content strategy and communicate it in a way that is clear and easily accessible to internal and external teams. Marketers can record their audience or persona insights and map out how their audiences typically interact with their brand throughout the buyer's journey. They will also be able to create content assignments for specific stages and personas and easily see content that has been created for each.
In the planning section of Skyword360, marketing leaders can view content that is being created across personas, stages, campaigns, channels, divisions, and regions. Views are easily filterable, and users can share and save views of the planner for increased ease of use. Team members across the enterprise can drill down to see the status of individual pieces of content and, based on permissions, can access completed content for reuse or translation.
With Skyword360, marketers can capture story ideas from internal and external team members, harnessing the collective brain power of organizations and beyond. If accepted, ideas can be assigned easily to content creators, whether they are internal team members or members of the Skyword freelance community. With customizable content templates and workflows, content, including social media posts, articles, e-books, images, videos, case studies, and infographics, can be created, reviewed, and edited. Keywords, tagging, and metadata can be applied within the platform so that content can be found easily, both internally and externally. Skyword360 is translated into 14 languages, and payments to freelancers can be made through the platform in any currency.
Marketers can preview and publish their content right from the platform across multiple channels, including their social accounts, website content management systems, and email campaigns.
Skyword360's digital asset manager provides a single repository to easily leverage assets that may otherwise be scattered across multiple locations and ensures brand consistency across the enterprise. With a DAM that is integrated into the content marketing system they already use, marketers are able to work within a one-stop shop that's scalable to the growth of their content operations.
With Skyword360, marketers can create personalized experiences for their customers and prospects by providing personalized recommendations both on their websites and through email and newsletters.
Skyword360 empowers marketers to measure and share the performance of all of their content through customizable dashboards, email performance snapshots, and robust reporting and analytics.
Download the Skyword360 Overview
Founded in 2010, Skyword is a leading content marketing software and services company whose customers have created and published more than one million original stories as articles, videos, images, infographics, podcasts, and animations on the Skyword Platform. These stories have earned Skyword customers more than two billion visits organically, and Skyword has paid its freelance creatives more than $30 million on behalf of its customers.
About Skyword
Skyword liberates brands from ineffective marketing practices and inspires them to create deeper connections with their audiences. Skyword360 makes it easy to produce, optimize, manage, and promote content at any scale to create personalized, lasting relationships. Skyword also provides access to a community of thousands of freelance writers and videographers, an editorial team, and program managers who help move clients' content marketing programs to new levels of creative excellence. The book Storynomics, authored by CEO Tom Gerace and globally recognized story expert Robert McKee, guides marketers through this approach. Skyword is a privately held company headquartered in Boston, MA. The company's technology center is located in Pittsburgh, PA. Current investors include Rho Acceleration, Cox Media Group, Allen & Company, Progress Ventures, and American Public Media Group. Skyword's customers include Abbott Laboratories, ADP, AutoTrader, GE Health, Glenmede, Groupon, HortonWorks, HP, Lahey Health, IBM, and other leading B2B and B2C brands.
https://www.skyword.com/press/skyword-announces-skyword360-powering-a-content-centric-approach-to-extraordinary-customer-experiences/ https://www.skyword.com/press/skyword-announces-skyword360-powering-a-content-centric-approach-to-extraordinary-customer-experiences/ Adam Giuriceo


text:
\section{Introduction}
\label{sec:intro}
The accretion of matter onto compact objects powers a wide variety of astrophysical phenomena, from X-ray binaries to active galactic nuclei.  When the accreting material has significant angular momentum, an accretion disk is formed around the gravitating center. The structure and spectrum of such disks depend essentially on the accretion rate $\dot{M}$. Three basic kinds of accretion regimes can be differentiated depending on how the actual accretion rate relates to the {\it critical rate} defined as,
\begin{equation}
  \dot{M}_{\rm crit} \equiv \eta \dot{M}_{\rm Edd} = \frac{L_{\rm Edd}}{c^2} \approx 1.4\times 10^{17} \frac{M}{M_{\odot}}\;\; {\rm g \;s}^{-1},
  \end{equation}
where
\begin{equation}
  L_{\rm Edd}=\frac{4 \pi G M m_{\rm p} c}{\sigma _{\rm T}}\approx 1.3\times10^{38} \frac{M}{M_{\odot}}\;\;{\rm erg\; s}^{-1}
\end{equation}
is the Eddington luminosity, $M$ is the mass of the accreting object, $\eta\approx 0.1$ is the radiative efficiency, and the rest of the symbols have their usual meaning. At sub-critical rates $\dot{M}\lesssim \dot{M}_{\rm crit}$ the disk is thin and can be described using the standard model developed by  \cite{shakura1973}. At very low accretion rates,  $\dot{M}<< \dot{M}_{\rm crit}$, optically-thin advection-dominated regimes are possible \citep[e.g.][]{narayan1994}. Finally, if the regime is super-critical, $\dot{M}>> \dot{M}_{\rm crit}$, the disk becomes optically-thick, geometrically slim or thick, and advection-dominated \citep[e.g.][]{paczynsky1980,abramowicz1980,calvani1981,wiita1982,beloborodov1998,fukue2000}.\par

It was already realized by \cite{shakura1973} that super-critical disks should expel a large amount of the accreting mass as optically thick winds. The generation, evolution, and appearance of such winds have been investigated by several authors \citep[e.g.][]{meier1979,fukue2009,fukue2011,kitabatake2002}. If a strong magnetic field is present in the inner part of the disk, super-critical sources can also launch well-collimated relativistic jets \citep{eggum1985,meier2005,fukue2005,okuda2005}. The resulting jet-wind interactions can be an important ingredient of the overall structure of the system. The wind is likely present at earlier stages of the evolution of the source, so the launching of the jet could even be inhibited if the wind is sufficiently dense. If the jet escapes, then wind collimation effects can also be significant \citep[see][]{globus2016}. An extremely powerful jet, on the other hand, might push sidewards the wind producing an equatorial outflow. This could be the case of the well-known super-accreting microquasar SS433, as the existence of an equatorial wind in SS433 has been revealed by high-resolution radio interferometric observations \citep{blundell2001,paragi2002} and the source has also powerful, precessing jets with hadronic content.\par

Another scenario where jet-wind interactions in super-critical sources might be crucial is that of Population~III microquasars (PopIII~MQs) \citep{romero2018}. In such binaries mass transfer from the very massive star to the black hole occurs through overflow of the Roche lobe, since PopIII~MQs have zero metallicity and no stellar winds. This leads to accretion rates that can exceed the Eddington rate by a factor of several thousands. These sources, then, are expected to be extreme super-critical accretors with very dense winds. The determination of how winds and jets interact in these objects is important because the resulting structure can present rather different properties depending on the jet and wind power relation. For instance, a narrow jet strongly collimated by a powerful wind may not be able to keep its integrity for long because of the growth of hydrodynamical instabilities. On the other hand, a broad jet and a quasi-equatorial wind could also lead to specific consequences because of the different impact on the ambient medium; note that jets in PopIII~MQs are expected to play a role in the cosmic re-ionization after the formation of the first stars \citep{sotomayor2019}.\par

In this paper we investigate the jet-wind interactions in super-critical microquasars of Population III using a combination of analytical models and numerical simulations. Our goal is to characterize the range of physical possibilities emerging from such interactions in systems with accretion rates largely exceeding the Eddington rate. In particular, we are interested in the formation of a quasi-equatorial outflow. \par
The structure of this paper is the following: in the next section we present the super-critical accretion disk models and their associated winds. Then, in Sect.~\ref{sect:Jet}, we outline the jet model we adopt, whereas we devote Sect.~\ref{sect:int} to the description of the simulations of the interactions and the results. From these findings, in Sect.~\ref{sect:PopIII}, we investigate the impact of an equatorial outflow on its environment. We close with a summary and some conclusions in Sect.~\ref{sect:concl}.

\section{Super-critical accretion disks and their winds}\label{sect:accretion}

The distinctive feature of super-critical accretion regime is photon-trapping in the disk \citep[see e.g.][]{,ohsuga2003,ohsuga2005}. When the photon diffusion time-scale exceeds the accretion time-scale, photons are advected towards the compact object without being able to go out from the surface. Advection of photons partially attenuates the disk luminosity. Following \cite{narayan1994}, the photon-trapping can be parameterized considering that advection heating is a fraction of the viscous heating, $Q_{\mathrm{adv}} = Q_{\mathrm{vis}} - Q_{\mathrm{rad}} = f Q_{\mathrm{vis}}$, where $Q_{\mathrm{rad}}$ is the radiative cooling rate, and $f$ is the advection parameter. In this paper, we assumed $f$ to be constant along the entire disk.

Powerful winds are expelled from the disk by the intense radiation pressure. We consider $\dot{M}>>\dot{M}_{\rm crit}$, so practically all the accreted matter is ejected through the winds \citep{fukue2000,fukue2004,lipunova1999}. A semi-analytical study of the physical properties of the super-critical accretion disk was developed by \cite{fukue2004} in the context of the \emph{critical accretion disk} model. In that model, it is assumed that the magnetization of the disk is weak enough to have no impact on the dynamics of the accreted fluid. However, it is expected that a toroidal magnetic field will be generated in the disk (for example, through the Biermann battery mechanism). The dynamics of the accreted fluid considering the effect of the toroidal fields is discussed in \cite{akizuki2006}. Accretion disks with toroidal magnetic fields launch winds but not jets, since the latter require a large-scale poloidal component of the field \citep{beckwith2008}.

The observational appearance of highly optically thick winds from super-critical sources has been examined by \cite{nishiyama2007}. In these outflows, the apparent photosphere (surface where the optical depth measured by an observer at infinity becomes unity) can extend up to thousands of times the gravitational radius of the central relativistic object. The wind provides an additional source of ultraviolet radiation and soft X-rays. \cite{sotomayor2019} showed that in the context of Population III microquasars, the emission from disk wind may be higher than the blackbody emission from the disk.

We consider that the initial velocity of the wind is a factor of the escape velocity (similar to stellar winds from massive stars) and neglect the self-gravitating effects of the disk. The mass-loss rate into the wind, per unit surface, is given by \citep[see][]{fukue2011}:

\begin{equation}
\rho v = \frac{1}{2\pi r}\frac{{\rm d}\dot{M}}{{\rm d}r}=\frac{\dot{M}_{*}}{2\pi r_{\rm cr}}\frac{1}{r},
\end{equation}
where $r_{\rm cr}$ is the critical radius defined in the Eq. (3) of \cite{fukue2004}\footnote{In the super-critical accretion regime, there exists some critical radius $r_{\rm cr}$ such that outside $r_{\rm cr}$, the accretion rate is constant and the disk is a radiation-pressure dominated standard disk. Inside
$r_{\rm cr}$, the accretion rate decreases with the radius as to maintain the critical rate, expelling the excess of mass by the radiation-driven wind \citep{fukue2004}.}. The critical radius is obtained by equating the radiation force and the vertical component of gravity (other possible forces on the plasma are neglected). The differential mass-loss rate does not depend on $r$: $d\dot{M}(r)/dr=\dot{M}_{*}/r_{\rm cr}$ \citep[see][]{fukue2004}.

In Table~\ref{table:Parameters} we show the parameters in the different models we are going to adopt to compute the various models. We note that the jet initial radius has been adjusted to comply with resolution limitations (see Sect.~\ref{sim}), although the mass, momentum, and energy dominance of the wind external regions leaves some freedom to set the value of this parameter. We have estimated the parameters of the disk using the model developed by \cite{sotomayor2019}. The disk is supposed to be in the optically-thick advection-dominated
state with toroidal magnetic fields. The viscosity parameter is $\alpha = 0.01$, constant along the entire disk. This is consistent with models of thick accretion disks in hydrostatic equilibrium \citep{jaroszynski1980} . The magnetic field is relatively strong, $\beta = p_{\rm gas}/p_{\rm mag} = 5$, and spread throughout the disk. Detailed formulae for the most relevant physical properties of the accretion disk (thickness, temperature, magnetic field,  velocity and spectral energy distribution of the emitted radiation) can be found in \cite{akizuki2006}. A sketch of typical super-critical accretion disk with winds is shown in Fig. \ref{fig:wind}.
\begin{figure}[h!]
\centering
\includegraphics[scale=.25]{wind_disk.pdf}
\caption{Scheme of the considered model of accretion disk and winds in super-Eddington microquasars. Toroidal magnetic fields are expected in the disk. As long as there is no poloidal magnetic field, there is no launching of jets. The figure corresponds to the parameters adopted in Sotomayor Checa \& Romero (2019).}
\label{fig:wind}
\end{figure}

\begin{table*}[t]
\centering \caption{\small Parameters of the models discussed in the text}
\label{table:Parameters}
\begin{tabular}{@{} ll}
\hline
Parameter [Unit] & Value\\
\hline
   $M_{*}$: Donor star mass [$M_{\odot}$] & $41$ \\
   $M_{\mathrm{BH}}$: Black hole mass [$M_{\odot}$]  & $34$ \\
   $a$: Orbital semiaxis $[R_{\odot}]$ & $36$ \\
   $\dot{M}_{\mathrm{*}}$: Mass-loss rate [$M_{\odot}\,\mathrm{yr}^{-1}$]  & $7.5\times10^{-5}$ \\
   $R_{*}$: Stellar radius $[R_{\odot}]$ & $14.2$ \\
   $r_{\mathrm{g}}$: Gravitational radius $[\mathrm{km}]$ & $50$ \\
   $\alpha$: Disk viscosity parameter & $0.01$  \\
   $f$: Advection parameter & $0.5$  \\
   $\beta$: Beta factor of the plasma & $5$  \\
   $r_{\rm cr}$: Critical radius $[r_{\mathrm{g}}]$ & $1.3\times 10^{4}$\\
   $L_{\rm disk}$: Disk luminosity $[\mathrm{erg\,s^{-1}}]$ & $10^{40}$\\
   $\chi$: Jet semi-opening angle tangent & $0.1$ \\
   $r_{\mathrm{0}}$: Jet initial radius $[r_{\mathrm{g}}]$ & $500$ \\
   $\dot{M}_{\mathrm{wind}}$: Total wind mass-loss rate $[M_{\odot}\,\mathrm{yr}^{-1}]$ & $7.3\times10^{-5}$ \\
   $\dot{M}_{\mathrm{jet}}$: Total jet mass-loss rate $[M_{\odot}\,\mathrm{yr}^{-1}]$ & $3.5\times10^{-7}$ \\
      \hline
   Case 1: Fast jet\\
   \hline
  $v_{\mathrm{wind}}$: Wind velocity & $\sqrt{2GM/r}$  \\
  $L_{\mathrm{wind}}$: Wind kinetic power $[\mathrm{erg\,s^{-1}}]$ & $10^{39}$ \\
  $\Gamma_{\mathrm{jet}}$: Jet bulk Lorentz factor & $9$ \\
  $L_{\mathrm{jet}}$: Jet kinetic power $[\mathrm{erg\,s^{-1}}]$ & $10^{41}$ \\
   \hline
   Case 2: Heavy jet\\
   \hline
  $v_{\mathrm{wind}}$: Wind velocity & $3\times \sqrt{2GM/r}$ \\
  $L_{\mathrm{wind}}$: Wind kinetic power $[\mathrm{erg\,s^{-1}}]$ & $10^{40}$ \\
  $\Gamma_{\mathrm{jet}}$: Jet bulk Lorentz factor & $1.35$ \\
  $L_{\mathrm{jet}}$: Jet kinetic power $[\mathrm{erg\,s^{-1}}]$ & $10^{40}$ \\
 \hline
 Case 3: Very powerful jet \\
 \hline
  $v_{\mathrm{wind}}$: Wind velocity & $9\times \sqrt{2GM/r}$ \\
  $L_{\mathrm{wind}}$: Wind kinetic power $[\mathrm{erg\,s^{-1}}]$ & $10^{41}$ \\
  $\Gamma_{\mathrm{jet}}$: Jet bulk Lorentz factor & $1.035$ \\
  $L_{\mathrm{jet}}$: Jet kinetic power $[\mathrm{erg\,s^{-1}}]$ & $10^{39}$ \\
 \hline
\end{tabular}
\end{table*}

\section{Jet model}
\label{sect:Jet}

If a large-scale poloidal magnetic field develops, highly collimated, oppositely directed relativistic jets are launched from the ergosphere of the black hole \citep[see e.g.][]{tchekhovskoy2015}. Jets in super-Eddington microquasars should drill the wind to escape. The matter in the jet comes from the accreted fluid in the disk, being injected first as neutral particles \citep{romero2020}. Although the wind can load the jet, we consider that the walls of the jet are impermeable (which is a good approximation for low pressures). In all cases, we assume a conical jet that it is ejected by conversion of magnetic energy into kinetic energy in a region close to the compact object, within the disk wind.\par

The magnetic field in the disk is initially only toroidal. A poloidal magnetic flux can be generated in situ through a turbulent dynamo powered by magnetorotational instabilities \citep{liska2018}. Then, the disk becomes a magnetically arrested disk or MAD in its inner region \citep{narayan2003}, and powerful jets are launched with Lorentz factor $\Gamma_{\rm jet} \approx 10$ \citep{sotomayor2019}. For a full discussion of the physics of these jets see e.g. \cite{romero2008}, \cite{romero2017} and \cite{romero2020}. Here we shall consider that the jets are perpendicular to the orbital plane and they do not precess. We shall investigate 3 different cases of jets. Case 1 is a fast jet launched by the black hole ergosphere. In Cases 2 and 3, we consider slower jets. These jets are similar to the case of SS433, the only known super-accreting galactic microquasar. Particularly, in Case 3 we adopt the Lorentz factor of the approaching jet of SS433. Finally, we consider that the jet is perpendicular to the orbital plane. All parameters of these models and the assumed values are shown in Table~\ref{table:Parameters}.

\section{Jet-wind interaction}
\label{sect:int}

We implement numerical simulations to explore the physics of the interaction between the jet and the wind of the accretion disk in super-Eddington microquasars. For PopIII~MQs, we consider different values of the jet Lorentz factor, fixing the mass-injection rate. The lower the Lorentz factor is, the lower results the kinetic luminosity of the jet (see Table~\ref{table:Parameters}). Also, varying the wind velocity we set the kinetic power of the wind. In Case 1, we consider that the wind velocity is given by the escape velocity $v_{\rm wind}(r) = v_{\rm esc} (r) = \sqrt{2GM/r}$. This implies  $L_{\rm wind}\approx 10^{39}\,{\rm erg\,s^{-1}}$ for $\dot{M}_{\mathrm{*}}=7.5\times 10^{-5}\,{\rm M_\odot\,yr^{-1}}$. In Cases 2 and 3, we adopt wind velocities higher than the escape velocity, resulting in $L_{\rm wind}\approx 10^{40}\,{\rm erg\,s^{-1}}$ for $v_{\rm wind}(r) = 3\,v_{\rm esc} (r)$, and $L_{\rm wind}\approx 10^{41}\,{\rm erg\,s^{-1}}$ for $v_{\rm wind}(r) = 9\,v_{\rm esc} (r)$ in Cases 2 and 3, respectively.

\subsection{Simulations}\label{sim}

We performed axisymmetric, relativistic hydrodynamical (rel. HD) simulations in 2 dimensions of the interaction between the jet and the super-Eddington wind. The jet thermal pressure is assumed to be $1$\% of the jet ram pressure divided by $\Gamma_{\rm jet}^2$, so the jet is very cold. The jet streamlines are radial, and the jet has a half-opening angle of 0.1~rad. To optimize the computational cost, the jet initial radius has been taken to be $500\,r_{\rm g}$. This value corresponds to $\approx 7$ cells. This is larger than the usual $\sim 10-100\,r_{\rm g}$ \citep[see e.g.][]{bosch-ramon2006}, but given that most of the wind mass, momentum and energy rates come from the larger radii, the results are not significantly affected. We remark that such an initial jet radius implicitly implies that the actual jet injection height, i.e. the distance from the disk mid-plane, must be larger than the radius. This means that the computational grid does not encompass the jet and wind formation zones, but it is assumed to capture the physics of these flows further downstream. In the perpendicular direction, however, the simulations start from the axis.\par

The wind is launched in the vertical direction for $r>500\,r_{\rm g}$. For $r>r_{\rm cr}$, the wind is injected as a flow of the same velocity than at $r\le r_{\rm cr}$, but with a much lower normalization for the density ($\times 10^{-4}$) and the pressure ($\times 10^{-6}$). Note that in a more realistic setup, instead of being purely vertical, the wind velocity field might start perpendicularly to the surface of the disk. In addition, the wind would carry angular momentum, which should also affect the evolution of the wind on larger scales. Here, however, we want to focus on the impact of the jet on the wind, and on the possibility of formation of an equatorial wind component. Thus, the cleanest way to make such a study as a first approximation is to assume a purely vertical wind.\par

The jet and wind total power, momentum and density rates adopted in theses simulations are those of Cases~1, 2, and 3, given in Table~\ref{table:Parameters}.\par

The code that solves the rel. HD equations is the same as in \citet{delacita2016}: third order in space; second order in time; and using the Marquina flux formula \citep{donat1996,donat1998}. Details on the fluid equations, the implementation of the spatial order scheme, and on the Riemman solver employed can be found in \cite{mignone2005}, \cite{donat1996} and \cite{donat1998}.\par

For the adiabatic index of the gas, we adopted a mono-atomic relativistic ideal gas value of $\gamma=4/3$, which corresponds to a suitable for the relativistic jet, and for an optically thick wind. This approximation fails in the region where the wind becomes optically thin, but for simplicity, we have kept that adiabatic index constant in the whole computational domain. We note that the fact that the wind is optically thick formally prevents efficient cooling, effectively implying that the wind is quasi-adiabatic with $\gamma\approx 4/3$. On the other hand, we assume that the jet is adiabatic, something that is the case under the densities and temperatures adopted in the simulation\footnote{One can still assume that some fraction of the jet energy can be in the form of radiating non-thermal particles, but we assume that such a component will not affect the jet dynamics.}. On larger scales, efficient cooling in an optically thin wind may lead to clumping, instabilities and even shocks, but the study of these effects is beyond the scope of this work.\par

For all cases investigated, the adopted computational grid consist of a uniform grid with 275 cells between $r=z=0$ and $r=z\approx 10^{11}$~cm ($\approx 2\times 10^4\,r_{\rm g}$ for $M_{\mathrm{BH}}=34\,M_\odot$). An extended grid is add with 125 cells in the $\hat{r}$- and $\hat{z}$-directions reaching $r=z=3\times 10^{11}$~cm ($\approx 6\times 10^4\,r_{\rm g}$ for $M_{\mathrm{BH}}=34\,M_\odot$). To avoid numerical artifacts, the $r$-to-$z$ cell aspect ratio is kept $\lesssim 10$ \citep{perucho2005}. Inflow conditions (the jet and the wind) are imposed at the bottom of the grid, reflection at the axis, and outflow in the remaining grid boundaries.\par

In the course of our study, we ran few tests with shorter simulations with two times more resolution and found that the results were consistent with those of the longer, lower resolution simulations. In any case, the first-approach aim of the simulations justify the modest levels of resolution adopted here. However, such a modest resolution can favor jet-wind lateral momentum transfer through numerical viscosity at the jet base, helping to form the equatorial wind. This probably happens in Case 1: the radial jet flow pushes laterally the wind flow, but numerical viscosity can also enhance this effect. We must nevertheless note that the same effect but with a physical (not numerical) origin may result from instability growth under more realistic conditions. In a much higher resolution simulation (beyond the scope of this work), the injection of small fluctuations, expected in the formation of the jet and the wind, both flows with high Reynolds numbers, should induce Kelvin-Helmholtz instabilities in the jet-wind interface leading to mixing of fluids and an effective viscosity.\par

\subsection{Results}

The simulations were run until they reached the steady state within the computational domain. The time needed to reach the steady state was approximately the time needed by the slowest flow in the simulation to cross the domain.
Different simulated times were needed for the jet-wind system to reach a stationary solution: 1112.3~s, 1686.4~s, and 2523.6~s, for Cases~1, 2, and 3, respectively. The slower the densest parts of the wind were, the longer the simulation was.

The density maps for all the cases studied are shown in Fig.~\ref{fig:sim}. The results show broader and narrower jets, and winds that are more or less deflected sidewards, depending on the jet-to-wind-power ratio.

For the case with dominant jet power (Case 1), the jet gets wider than its initial opening angle, getting somewhat recollimated at higher heights, and the wind develops a strong equatorial component. For the intermediate and dominant wind cases (Cases 2 and 3), the jet is well-collimated and the wind keeps mostly vertical.

We have computed the average angle with respect to the $\hat{r}$-direction (i.e. the symmetry plane) at which the wind mass is leaving the grid, and obtained: $44.4^\circ$, $58.2^\circ$, and $58.4^\circ$, for Cases 1, 2, and 3, respectively. Recall that there should be a counter-wind in the $-\hat{z}$-direction, and that lateral jet-wind momentum transfer occurring on larger scales of the structure may lead to somewhat stronger collimation towards the symmetry plane, with the consequent merging of the two wind components in that plane. Thus, it is expected that for Case 1 the wind will look more like a broad equatorial flow than like a vertical one\footnote{The equatorial wind in Population III microquasars does not stop accretion. In these systems the accretion is by overflowing the Roche lobe, therefore the accreted matter flows only in the plane where the Lagrange point is contained, while the equatorial wind is always directed above the accretion disk. On the contrary, accretion arrest could occur if mass transfer from the star is by stellar winds, as in Population I microquasars.}. For Cases 2 and 3, the impact of the jet is smaller; Fig.~\ref{fig:sim} (bottom) basically shows a somewhat widened flow strongly directed upwards.

In a realistic scenario the jet properties may be different from those found here. We are computing a steady solution of the dynamics of the jet-wind system, although some variability is expected in the injection of both structures, which will surely lead to instability growth downstream the jet. Given that jet variability in super-Eddington accreting sources is beyond the scope of our work, we leave the numerical analysis of such a scenario for future research. In the following sections we consider the effects of a quasi-equatorial wind in PopIII~MQs (Case~1). Since a quasi-equatorial outflow emerges by the influence of the jet on the wind, we refer to it hereafter as the \textit{jet-induced wind}.
\begin{figure}[h!]
\centering
\hspace*{-1cm}
  \begin{minipage}{0.5\textwidth}
\centering
    \includegraphics[scale=.6]{cas1.png}\\
   \end{minipage}%
  \hspace{5mm}
  \begin{minipage}{0.48\textwidth}
    \centering
 \hspace*{-1.cm}
    \includegraphics[scale=.6]{cas2.png}\\
  \end{minipage}
    \hspace{5mm}
  \begin{minipage}{0.48\textwidth}
    \centering
    \hspace*{-1.cm}
    \includegraphics[scale=.6]{cas3.png}\\
  \end{minipage}
  \caption{Colored density maps (the color scale units are erg~cm$^{-3}$, corresponding to $\rho c^{2}$) of Cases 1 (top), 2 (middle), and 3 (bottom). For the jet and wind parameters, see Table~\ref{table:Parameters}.}
      \label{fig:sim}
\end{figure}
\section{Interaction between the jet-induced wind and the donor star}
\label{sect:PopIII}
\subsection{Stagnation of the wind}
From the results obtained in our simulations, we can estimate the velocity of the jet-induced wind at the end of the grid as $v_{\rm w} \approx 3.7\times 10^{8}\,{\rm cm\,s^{-1}}$. We assume that this supersonic velocity is the terminal value.\par

Part of the jet-induced wind flows towards the donor star along the orbit. Since Population III stars have no winds, they are metal-free, the wind can only be stalled by the stellar radiation pressure. The radiation pressure balance the ram pressure of the wind at the point given by:
\begin{equation}
\rho_{\rm w}(r_{\rm \small BH})\,v_{\rm w}^2 = P_{\rm rad} \approx \frac{L_{*}}{12\pi cr_{\rm \small S}^{2}},
\end{equation}
where an optically thick wind is adopted, $r_{\rm \small BH}$ is the distance to the stagnation point measured from the black hole, and $r_{\rm \small S}$ is the distance measured from the star.\par

In the supersonic wind region, the density varies with radius according to $\rho_{\rm w} = \rho_{\rm w,0} (r_{0}/r)^{2}$, where $\rho_{\rm w,0}$ and $r_{0}$ are values at some reference point. We adopt $\rho_{\rm w,0} = 10^{-12}\,{\rm g\,cm^{-3}}$, $r_{0} = 3\times10^{11}\,{\rm cm}$ (see Case 1 in Fig.\ref{fig:sim}), and $ L_{*} = 3\times10^{6}L_{\odot}$. Replacing, we obtain $r_{\rm \small S} \approx 17\,R_{\odot} \approx 1.2\,R_{*} > R_{*}$, then the jet-induced wind is halted by the radiation pressure of the star. This occurs because the luminosity of the first stars is extremely high. Shocks and the associated radiation are expected from this stagnation region of the wind. A forward shock propagates in the tenuous medium dominated by stellar radiation, and a reverse shock moves back towards the black hole. In what follows, we investigate the possibility of particle acceleration in the reverse shock by diffusive shock acceleration, which requires adiabatic conditions to be fullfiled. A sketch of the interaction between the wind and the donor star is shown
in Fig.\ref{fig:interaction}. \par

\begin{figure}[h!]
\centering
\includegraphics[scale=.28]{sketch2.pdf}
\caption{Scheme of the interaction between the equatorial wind and the donor star. The wind stagnates at the point where $\rho_{\rm w} v_{\rm w}^2 = P_{\rm rad}$. The distances from the stagnation point to the black hole and the center of the star are indicated as $r_{\rm \small BH}$ and $r_{\rm \small S}$, respectively.}
\label{fig:interaction}
\end{figure}

\subsection{Particle acceleration}

The parameter that determines whether a shock may be treated as adiabatic is the thermal cooling length of the medium traversed by the shock. If the length scale of the medium is higher than the thermal cooling length, the shock is adiabatic, otherwise it is radiative. A detailed discussion of the nature of shocks and their ability to accelerate particles is given in \cite{muller2020}. The thermal cooling length of the wind is given by \citep{mccray1979}:

\begin{equation}
R_{\Lambda} = \frac{5.9\times 10^{-11} \mu \left(v_{\rm sh}/{\rm km\,s^{-1}} \right)^3}{\left(n_{\rm w}/{\rm cm^{-3}} \right)\left(\Lambda(T) / {\rm erg\,s^{-1}\,cm^{-3}} \right)}\;{\rm cm},
\end{equation}
where $\mu = 0.6$ for a fully ionized plasma, $v_{\rm sh} \approx 4\,v_{\rm w}/3$ is the velocity of the reverse shock, $n_{\rm w}$ is the density of the wind in the pre-shocked region, $T = 20 \mu  \left(v_{\rm sh}/{\rm km\,s^{-1}} \right)^2$, and $\Lambda (T)$ is the cooling function. Then, we obtain $v_{\rm sh} \approx 5000\,{\rm km\,s^{-1}}$, and $T \approx 3\times10^8 \,{\rm K}$. For this temperature value, the cooling function is given by \citep{wolfire2003}:
\begin{equation}
\Lambda (T) = 3\times 10^{-27} T^{0.5},
\end{equation}
so, $\Lambda \approx5.2\times 10^{-23}\,{\rm erg\,s^{-1}\,cm^{-3}}$. Replacing, the thermal cooling length is $R_{\Lambda} \approx 10^{12}\,{\rm cm}$.\par
This length scale is on the order of the size of the jet-induced wind, measured from the stagnation point to the black hole. If we consider that the particle acceleration occurs in a small region around the reverse shock, the adiabaticity condition of the reverse shock is guaranteed. We adopt a thickness of $\Delta x_{\rm acc} = 1.2\times10^{8}\,{\rm cm} \left(\approx 3\times 10^{-5}\,r_{\rm \small BH} \right)$ for the particle acceleration zone, so that the ambient fields can be assumed to be homogeneous. Accordingly, we calculate the acceleration and cooling rates of relativistic particles in a stationary one-zone model, for scenarios of efficient and inefficient acceleration in the reverse shock. The adopted parameters are listed in Table \ref{table:wind parameters}.\par

\begin{table*}[t]
\centering \caption{\small Parameters of the particle acceleration region close to the stagnation point of the equatorial outflow.}
\label{table:wind parameters}
\begin{tabular}{@{} ll}
\hline
Parameter [Unit] & Value \\
\hline
   $L_{\mathrm{K}}$: Kinetic power of the jet-induced wind [$\mathrm{erg}\,\mathrm{s}^{-1}$]& $1.7\times 10^{37}$ \\
   $v_{\mathrm{wind}}$: Equatorial wind velocity [${\rm cm\,s^{-1}}$] & $3.7\times 10^{8}$\\
   $\theta$: Wind semi-opening angle & $27$$^{\circ}$ \\
   $q_{\mathrm{rel}}$: Content of relativistic particles & $0.1$\\
   $\zeta$ Hadron-to-lepton energy ratio & $1$ \\
   $r_{\rm \small S}$: Acceleration point from the center of the star [${\rm cm}$] & $1.2\times10^{12}$ \\
   $r_{\rm \small BH}$: Acceleration point from the black hole [${\rm cm}$] & $4.3\times10^{12}$ \\
   $B$: Magnetic field at the acceleration point [$\mathrm{G}$] & $60$ \\
   $n_{\mathrm{p}}$: Cold matter density at the acceleration point [${\rm cm^{-3}}$] &  $6.7\times 10^{10}$\\
   $\Delta x_{\mathrm{acc}}$: Size of the acceleration region [${\rm cm}$] & $1.2\times 10^{8}$ \\
   $p$: Injection spectral index & $2.2$\\
   $\eta_{\rm acc}$: Acceleration efficiency & $10^{-4}\,-\,10^{-1}$ \\
   $E_{\mathrm{e}}^{\mathrm{min}}$: Minimum electron energy [$\mathrm{MeV}$] & $1$  \\
\hline
\end{tabular}

\end{table*}

In the acceleration region, a small fraction of the total kinetic power of the jet-induced wind is transferred to relativistic particles by diffusive shock acceleration: $ L_{\mathrm{rel}} = q_{\mathrm{rel}}L_{\mathrm{K}}$. We assume equipartition between relativistic electrons and protons $L_{\mathrm{p}} = \zeta \,L_{\mathrm{e}} = L_{\mathrm{e}}$. The particle injection function is a power-law in the energy $Q(E,z) = Q_{\mathrm{0}}{E^{-p}}$, where $p$ is the spectral index $\sim 2$. The maximum energy $E^{\mathrm{max}}$ that a relativistic particle can attain is obtained by balancing its acceleration and cooling rates (including advection effects).
\par
The acceleration rate for a charged particle in a magnetic field $B$ is:
\begin{equation}
t_{\mathrm{acc}}^{-1} = \frac{\eta_{\rm acc} e c B}{E},
\end{equation}
where $E$ is the energy of the particle, $\eta_{\rm acc}$ is a parameter that characterizes the efficiency of the acceleration mechanism, and the magnetic field in the acceleration region is given by $B = B_{*}\left(R_{*}/r_{\rm \small S}\right)^{3}$, where $B_*$ is the surface magnetic field of the star\citep[see][]{reimer2006}\footnote{The particle acceleration rate depends on the shock velocity and the diffusion coefficient of the medium. For both shocks parallel or perpendicular to the magnetic field, the diffusion coefficient is a multiple of the Bohm diffusion coefficient, therefore the acceleration timescale is inversely proportional to the gyroradius of the particles \citep[See][]{drury1983}.}. We adopt $B_{*} = 100\,{\rm G}$, similar to the reported for O and B stars in the local Universe \citep{mathys1999}.\par

The total cooling rate is the sum of the radiative cooling rates and adiabatic loss rate $t_{\mathrm{cool}}^{-1} = t_{\mathrm{rad}}^{-1} + t_{\mathrm{ad}}^{-1}$. The adiabatic losses are caused by the expansion of the acceleration region and the radiative losses by the interaction of the relativistic particles with the ambient fields. We consider electron losses by synchrotron radiation, inverse Compton scattering and relativistic Bremsstrahlung, and proton losses by synchrotron radiation, inelastic proton-proton collisions, and photo-hadronic interactions. The target protons for $pp$ collisions and relativistic Bremsstrahlung interactions are the cold protons in the shocked wind, and the target photons for inverse Compton scattering and $p\gamma$ collisions are provided by the radiation field of the star. This field is so strong, that makes all other radiation field sources negligible.
\par
Figures \ref{fig:times electrons} and \ref{fig:times protons} show the cooling and acceleration times in the acceleration region. For $E_{\rm e} < 1\,{\rm GeV}$, the electrons are advected by the shocked wind and escape of the acceleration region without radiative cooling. For $E_{\rm e} > 1\,{\rm GeV}$ electrons cool before escaping by inverse Compton scattering. If the acceleration mechanism is inefficient, the electrons only interact with the photons of the stellar radiation field in the Thomson scattering regime. Otherwise, the electrons reach much higher energies, and are cooled by Compton scattering in the Klein-Nishina regime and synchrotron radiation emission. Protons in any case escape from the acceleration region without cooling, therefore the non-thermal spectrum will be dominated by leptonic processes.
\par
\begin{figure}[h!]
\centering
\includegraphics[scale=0.33]{electron_cooling.pdf}
\caption{\small Rates of acceleration and radiative losses for electrons.}
\label{fig:times electrons}
\end{figure}
\begin{figure}[h!]
\centering
\includegraphics[scale=0.33]{proton_cooling.pdf}
\caption{\small Rates of acceleration and radiative losses for protons.}
\label{fig:times protons}
\end{figure}
We solve the transport equation for electrons considering efficient and inefficient acceleration. In Figs. \ref{fig:distribution high efficiency} and \ref{fig:distribution low efficiency} we show the distributions of electrons in steady state in the one-zone model. At low energies, the spectral index of the distribution does not differ from that of the injection function because particle escape dominates. When the radiative processes significantly cool the particles, the spectral index changes, initially producing a softening in the spectrum (when Thomson scattering dominates), then a hardening (in the Klein-Nishina regime), and finally it softens again (mainly because of synchrotron losses).
\par
\begin{figure}[h!]
\centering
\includegraphics[scale=0.33]{electron_distribution_1.pdf}
\caption{Distribution of relativistic electrons in the stationary one-zone model for a highly efficient acceleration.}
\label{fig:distribution high efficiency}
\end{figure}
\begin{figure}[h!]
\centering
\includegraphics[scale=0.33]{electron_distribution_2.pdf}
\caption{Distribution of relativistic electrons in the stationary one-zone model for a low value of acceleration efficiency.}
\label{fig:distribution low efficiency}
\end{figure}
\subsection{Nonthermal emission}
Interactions of the relativistic electrons with the ambient fields give rise to broadband radiation mainly dominated by synchrotron and inverse Compton. The efficiency of the acceleration mechanism determines the high-energy cut-off of the spectrum. Regardless of $\eta_{\rm acc}$, the radiation is totally suppressed for energies $10\,{\rm GeV} < E_{\gamma} < 10\,{\rm TeV}$ by annihilation with photons of the stellar radiation field, as shown in Fig. \ref{fig:attenuation factor}. In addition, internal absorption partially attenuates the emission of $\gamma$ rays for $E_{\gamma} > 1\,{\rm TeV}$. Most of the radiation, however is produced at lower energies.
\par
\begin{figure}[h!]
 \centering
 \includegraphics[scale=0.33]{attenuation.pdf}
    \caption{\small Attenuation factor of the emitted radiation by $\gamma \gamma$-annihilation. Internal absorption is caused by interaction with the photons created in the acceleration region by the nonthermal radiative processes. The external stellar radiation field provides the target photons for stellar absorption.}
       \label{fig:attenuation factor}
 \end{figure}
The resulting nonthermal spectrum is shown in Fig. \ref{fig:total SED}, including the radiative processes of the first generation of secondary pairs. The absorbed radiation is re-radiated up to energies of 1 TeV by Compton scattering. The processes of $\gamma \gamma$-annihilation, pair creation, and emission of very-high-energy photons by inverse Compton scattering occur only on scales of the binary system.\par
Gamma rays from the inner jet are suppressed for $E_{\nu} > 100\,{\rm MeV}$ by internal absorption \citep{sotomayor2019}. We show here that, nevertheless, photons with energies up to $E_{\gamma} = 1\,{\rm TeV}$ can be expected on binary system scales if the shocks produced by the jet-induced wind can efficiently accelerate particles. Electromagnetic cascades by the interaction of the gamma rays with the cosmic microwave background inject additional high-energy particles in the binary environment.\par
The results shown above do not depend significantly on the size of the acceleration region. In the limit case of considering the entire region between the stagnation point and the surface of the star as the acceleration zone, the proton escape time is still smaller than the radiative cooling time, so a leptonic model is still adequate.\par
For details on the calculation of the cooling rates, emissivities, and opacities, the reader is referred to \cite{bosch-ramon2006,romero2008,romero2010}; and references therein.\par
\begin{figure}[h!]
 \centering
 \includegraphics[scale=0.33]{total_SED.pdf}
    \caption{\small Spectral energy distribution of the nonthermal radiation emitted in the acceleration region. Nonthermal radiative processes of the secondary pairs are considered for the calculation of the total spectrum.}
       \label{fig:total SED}
 \end{figure}
\section{Summary and conclusions}\label{sect:concl}
We have implemented relativistic hydrodynamical simulations in order to characterize the jet-wind interaction in microquasars with super-Eddington accretion rates. We have applied our study to PopIII~MQs. In order to model the jet-wind interaction in these objects we have adopted the model developed by \cite{sotomayor2019}.\par

We found that the main parameter that determines the jet-wind structure in PopIII~MQs is the relative kinetic power. We have explored three different posibilities: $L_{\rm jet} = 10^{-2}\, L_{\rm wind}$, $L_{\rm jet} = L_{\rm wind}$, and $L_{\rm jet} = 10^{2}\, L_{\rm wind}$. When $L_{\rm jet} << L_{\rm wind}$ (Case 3) or $L_{\rm jet}\sim L_{\rm wind}$ (Case 2), jets keep narrow while the winds do not get significantly deflected sidewards. In such a case, the system is a powerful source of UV radiation and soft X-rays emitted by the wind, and one would expect strong variability of the jet induced by possible wind changes (not explored numerically here). If the kinetic power is similar for both jets and winds, $L_{\rm jet} \approx L_{\rm wind}$, the jet
may still be somewhat powerful enough to compete with the wind in luminosity, if efficient particle acceleration takes place in the jet. For the case when the kinetic power of the jet is greater than that of the wind, $L_{\rm jet} >> L_{\rm wind}$, the jet strongly affects the structure of the wind, which becomes equatorial and the jet escapes almost without being perturbed. In this case, the jet is the most prominent source of radiation for a distant observer.\par

The geometry we have adopted for the wind of the accretion disk is a purely axisymmetrical flow. In this way, we can analyze more adequately the production of a jet-induced equatorial wind. However, a more realistic geometry should take into account a wind that interacts collisionally with the jet. This would lead to shocks in the jet and to a decrease in jet velocity, likely reducing the capacity of the jet to emerge from the binary system.\par

It is evident that if the luminosity of the Population III star is lower than assumed, the stellar radiation pressure would not halt the equatorial wind. For example, if $L_{*} = 10^{6}L_{\odot}$, then $r_{\rm \small S} \approx 13\,R_{\odot} \approx 0.92\,R_{*}$. In this case, the wind is stopped at the surface of the star. This problem has been studied by \cite{usov1992}, in the context of colliding-wind binaries.\par

When the radiation pressure of the star stagnates the equatorial wind, and a consequent efficient acceleration of particles takes place in the reverse shock, very-high energy gamma rays are injected on scales of the binary system. Electron-positron pairs are created by annihilation, and are expected to deposit their energy at large distances from the binary system. These produce a new reionization channel that should be investigated with numerical simulations.\par

Since in Population III microquasars no appreciable amount of metals is expected in the disk, the radiation drives the wind by Thomson scattering and not by spectral lines as in massive stars in the local Universe. Therefore, we can assume that the wind accelerates only in the lower layer and quickly reaches its terminal velocity, since beyond that the scattered radiation transfers momentum to the wind almost isotropically. This justifies the hydrodynamic treatment at scales of the jet-wind interaction region. Radiation-hydrodynamical simulations are necessary to analyze the same problem in enriched disks.\par

The precession of the jet should increase the transfer of momentum to the wind and modulate it with the precessional phase. A faster wind might be produced that could deposit the bulk of its energy at long distances from the binary system, for example, when interacting with outer dense regions. Our model of jet-induced wind provides a simple mechanism for generating an supersonic equatorial outflow. If this wind is optically thick enough, it can hide the accretion disk and the donor star, as reported in SS433 \citep[see][]{fabrika2004}.\par

Along with wind variability, we have not considered here the effect of baryon loading of the jet by the wind. The simulations consider only one species of particles. However, baryon loading by the wind may be relevant in hadronic microquasars like SS433, where the presence of nuclei in the jets has been revealed through the detection of Fe-lines \citep{migliari2002}. We plan to investigate all these effects and report the results in a future paper.

\acknowledgments
PSC is Fellow of CONICET and PhD student at Universidad Nacional de La Plata (UNLP). PSC thanks the UNLP for the training received during his undergraduate studies, and the public education system in Argentina. GER is very grateful to the ICCUB where part of this research was done. This work was supported by the Argentine agency CONICET (PIP 2014-00338) and the Spanish Ministerio de Ciencia e Innovaci\'on (MICINN) under grant PID2019-105510GBC31 and though the "Center of Excellence Mar\'ia de Maeztu 2020-2023" award to the ICCUB (CEX2019-000918-M). V.B-R. is Correspondent Researcher of CONICET, Argentina, at the IAR.

\bibliographystyle{spr-mp-nameyear-cnd}

redpajama_set_name: RedPajamaArXiv


Spring Peeper Farm: The Great Escape!
Dave is so proud of his mink proof chicken coop. What he didn't realize that if a mink can't get in, then nothing can get out! Including his claustrophobic wife!
J. has had it drilled in his head, lock the chicken door behind you...lock the chicken door behind you! Well he locked the chicken door behind him alright and I was in it!! I never noticed he had locked the door until it was time for me to go inside. By then it was too late.
He was in the house...all the windows are closed of course...it's WINTER! So I begin to slowly freak out. Just slowly. I look at the chickens and they're just staring at me. I know they're thinking feed me or we'll feed on you!
So I begin to yell...and yell...and yell some more...then I start to scream and screech!! I'm feeling my voice going hoarse.
The panic starts to set in fast now. Nobody is hearing me. Come on people...it's a clear winter's night. No wind, nothing. My voice should carry all the way to Manitoba for Pete's Sake! But nobody heard me.
So I start to bang on the door, and bang and bang! Nothing. The door is solid.
So I try to bust the door down with my foot. It looks so easy in the movies! You'd think it would be even easier with a screen door. Ah....no. It's not easier, the screen stretches!
Dear hubby builds things to last. You'd think he built it for a bear...not a few chickens and minks or a wounduptighterthanaspring wife!. Criminy!
By this time I AM HYSTERICAL!!! It's been 30+ minutes.
Finally Dave realizes I've been outside for longer than necessary and comes to my rescue.
I'm not proud to admit it, but I really am hysterical and crying by now. But after going inside I finally calmed down. J. felt so bad. But it wasn't his fault. For once...he listened!
I'd be hysterical too. My hubby probably wouldn't even think to check!


During the next few years, the Ford Transit van will replace the Ford's Econoline range as the base vehicle of choice for ambulance operators, shuttle bus fleets and other commercial and public sector customers. It seems likely that Ford may completely phase out the 50-year-old Econoline lineup.
A version of the new Transit van, which is already available in Europe, will be replacing the Econoline in North America.
Ford will migrate its commercial vans around the world to a common Transit global platform in 2013 making the Transit a global cargo and people hauler. Kansas City Assembly Plant workers will soon begin producing the full-size Transit for North American customers.
Speaking recently at a Detroit auto event where the Ford Transit was being showcased, James D. Farley Jr., who is executive vice president of Global Marketing, Sales and Service and Lincoln at Ford said: "There will be a transition period away from the Econoline," and referring to vehicles converted to ambulances and shuttle buses etc. added "The cutaway business is extremely important, and we want to maintain customer choice while we go through that process. But eventually, we want to be down to one commercial van."
Ford plan to offer a 3.2-litre diesel 5-cylinder engine which should result in at least a 25% better fuel economy than similar Econoline vans. Anyone who has ever driven an Econoline van in the US will certainly know that this will be very welcome news for van owners in North America!


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Moris Hju Frederik Vilkins (; Novi Zeland, 15. decembar 1916 — 5. oktobar 2004) je bio engleski fizičar i molekularni biolog." Njegova istraživanja su doprinela naučnom razumevanju fosforescencije, izotopne separacije, optičke mikroskopije i difrakcije X-zraka, kao i razvoju radara. On je najbolje poznat po radu na Kings koledžu u Londonu na strukturi DNK. Kao znak priznanja za njegov rad, on je zajedno sa, Fransisom Krikom i Džejmsom Votsonom nagrađen Nobelovom nagradom za fiziologiju ili medicinu 1962. "za njihova otkrića molekulske strukture nukleinskih kiselina."

Reference

Literatura
-{
 Robert Olby; 'Wilkins, Maurice Hugh Frederick (1916–2004), Oxford Dictionary of National Biography, online edn, Oxford University Press, Jan 2008
 Robert Olby; "Francis Crick: Hunter of Life's Secrets". ., published in August 2009.
 John Finch; 'A Nobel Fellow On Every Floor', Medical Research Council. .; this book is all about the MRC Laboratory of Molecular Biology, Cambridge
 Robert Olby; "The Path to The Double Helix: Discovery of DNA"; first published in October 1974 by MacMillan, with foreword by Francis Crick. ; the definitive DNA textbook, revised in 1994, with a 9 page postscript.
 Horace Freeland Judson, "The Eighth Day of Creation. Makers of the Revolution in Biology"; CSHL Press. .
 Watson, James D. The Double Helix: A Personal Account of the Discovery of the Structure of DNA; The Norton Critical Edition, which was published in 1980, edited by Gunther S. Stent. .
 Chomet, S. (Ed.), D.N.A. Genesis of a Discovery, 1994, Newman- Hemisphere Press, London; NB a few copies are available from Newman-Hemisphere at 101 Swan Court, London SW3 5RY (phone: 07092 060530).
 Maddox, Brenda, Rosalind Franklin: The Dark Lady of DNA. .
 Sayre, Anne Rosalind Franklin and DNA. .
 Wilkins, Maurice, The Third Man of the Double Helix: The Autobiography of Maurice Wilkins. .
 Crick, Francis, What Mad Pursuit: A Personal View of Scientific Discovery (Basic Books reprint edition).
 Watson, James D., The Double Helix: A Personal Account of the Discovery of the Structure of DNA, Atheneum.  (first published in 1968)
 Krude, Torsten (Ed.) DNA Changing Science and Society: The Darwin Lectures for 2003 CUP 2003, includes a lecture by Sir Aaron Klug on Rosalind Franklin's involvement in the determination of the structure of DNA.
 Ridley, Matt; "Francis Crick: Discoverer of the Genetic Code (Eminent Lives)" was first published in June 2006 in the US and then in the UK September by HarperCollins Publishers. ; this short book is in the publisher's "Eminent Lives" series.
 "Light Is A Messenger, the life and science of William Lawrence Bragg" by Graeme Hunter.
 "Designs For Life: Molecular Biology After World War II" by Soraya De Chadarevian. ; it includes James Watson's "well kept open secret" from April 2003!
 Tait, Sylvia & James "A Quartet of Unlikely Discoveries".
}-

Spoljašnje veze

 Moris Vilkins
 Govor na Nobelovoj ceremoniji 1962.

Рођени 1916.
Умрли 2004.
Биофизичари
Нобеловци за медицину
Енглески физичари
Молекуларни биолози
Британски физичари
Пројекат Менхетн
Британски нобеловци
Новозеландски нобеловци
Новозеландски физичари


What does it mean to 'downshift'? Why is it now imperative that millions of people begin moving towards a simpler, more sustainable lifestyle ? If you, too, are to join this worldwide effort to create a different sort of world, when should you start? How should you set about it? Might you need to move house in order to live more sustainably, and if so, to where? And to whom can you turn for advice and guidance? This easy-to-read guidebook, by an author who undertook a similar journey, aims to answer all these questions and more. It will reassure you that while the downshifting process is not without its challenges, the rewards, in terms of life satisfaction, enjoyment and sense of fulfilment, can be huge. There are many books full of practical ideas for green living. But this one goes to the heart of the matter by looking at who you are, what your needs are and how to create your custom-made plan for a lifestyle perfectly adapted to the coming 'Age of Sustainability'.


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Pittsburgh Pirates 2022 Season Betting Preview: Win Totals and NL Central Futures Odds
Written By Nathan Frederick on March 28, 2022 - Last Updated on April 4, 2022
The Pittsburgh Pirates are projected by oddsmakers at PA sportsbooks to be one of the worst teams in baseball in 2022. It's not surprising this ship is at the bottom of Major League Baseball with a projected $37.9 million payroll, one of the lowest in the league.
There are other – more reasonable ways – to bet on the Pirates besides the longshot odds to win the World Series or National League Pennant.
Depending on how you think the Pirates will fare with their budget roster, you can wager on if they will go over or under their win total. And there will be chances to cheer and raise the Jolly Roger. Oneil Cruz is an early contender for NL Rookie of the Year. However, the shortstop will start the season in Triple-A.
Pittsburgh Pirates 2022 odds World Series, NL Pennant, NL Central
The Pittsburgh Pirates have not won a World Series since 1979 and they haven't the playoffs since 2015.
Oddsmakers are expecting the Milwaukee Brewers to repeat as NL Central Champions (-165 at DraftKings PA Sportsbook) and the Los Angeles Dodgers (+230) are the favorites to win the National League Pennant.
Pittsburgh Pirates win total odds
FanDuel PA sportsbook set Pirates win total at 64.5 wins, the lowest win total of any team.
Pittsburgh Pirates record over the last 10 years
2021: 61 – 101
2020: 19 – 41 (COVID-shortened season)
2019: 69 – 93
2015: 98 – 64 (clinched Wild Card)
Pittsburgh Pirates playoff odds
The Pirates will need a lot of things to fall into place to make the playoffs in 2022. A lineup that has a lot of question marks will need to produce. A pitching staff that lacks dominant starters must perform well.
At present, DraftKings has the Pirates at +1800 to make the playoffs. A "No" wager on the playoffs is -10000.
Oneil Cruz Rookie of the Year odds
Oneil Cruz will not start the 2022 season on the Pittsburgh Pirate's Opening Day roster. The 23-year old shortstop was sent to Triple-A to get "a little more experience" according to manager Derek Shelton. Cruz played two games in the majors last year. As of March 31, PA sportsbooks list Cruz as one of the favorites to win NL Rookie of the year. Cruz is +400 at BetMGM, second to the favorite Seiya Suzuki (+350). At DraftKings, Cruz is +380.
2022 Pittsburgh Pirates player prop season betting preview
Outfielder Bryan Reynolds figures to be one of the Pirates' best players this season. Last year, he hit .302 with 169 hits, 24 home runs and 90 RBI. In futures bets, he's +2800 at DraftKings to lead the league in hits this year.
DraftKings also has a prop bet based on his season hit total.
Bryan Reynolds Regular Season Total Hits props
Over 156.5: -110
Under 156.5: -110
2022 NL Central Odds
Surprisingly, the Pirates have not won the National League Central since the division was created in 1994. The odds are not in the team's favor this year either, with most sportsbooks setting the Pirates' odds to win the NL Central near +5000.
Lead image Philip G. Pavely/AP
Nathan Frederick
Nathan Frederick is an award-winning writer with more than 1,000 published bylines and two decades of journalism experience. His work has won awards from the Pennsylvania Society of Professional Journalists, the Keystone Press Association, and the Associated Press Sports Editors. He has also authored three books, one of which debuted as an Amazon No. 1 New Release.
View all posts by Nathan Frederick


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Just 5 minutes from Shinjuku by train and located in the center of Tokyo, this hotel has great access to transportation whilst still providing a comfortable stay in the quiet neighborhood.
From Akebonobashi Station (Toei Shinjuku Line) Exit A3: About 3 min on foot.
From Yotsuya-sanchome Station (Tokyo Metro Marunouchi Line): About 10 min on foot.
From Ichigaya Station (JR Sobu Line): About 12 min on foot.
From Shinjuku Station: About 10 min by taxi.


ofis is a brand-new 4,000 sq. ft coworking space in Mar Vista, opened in the 2015 spring, conveniently located few minutes away from the 405 & 10 highways and Venice beach.
It's a community as well: besides regular events/workshops, working around other freelancers and talented professionals is a unique opportunity to collaborate, be inspired, stay motivated and grow your business.


Sunday May 23rd was the second annual Healthy Habits Day put on by the Oregon State University Community Service Center. It was held at Community Outreach Inc. a different venue from last year's event, which was held at OSU's Dixon Recreation Center. The idea this year was to work with a community organization to help educate the general public about different ways they could incorporate healthy habits into their daily lives to help foster their well being. How do you do that you ask? Well we had Community Outreach Inc. participate by inviting their underserved community to the event, also organizations form Oregon State University and OHSU joined us to help put on the event. Among the groups was the Pre-Pharmacy club, OSU Dietician Ann Merchant and OHSU helped by lending exhibits to the event as well. Participants walked around the set up of interactive exhibits and nutritional information tables learning different facts about the ingredients in many popular foods and additives of some popular snacks such as Nutri-Grain bars and soda beverages. There were also exhibits that related to serving portions and measuring physical condition through a sit-up challenge designed for children. This was our first attempt at relocating an event off of the OSU campus to help the larger Corvallis community, and it was a success, we are eager to partner with other organizations from around the city and OSU to continue to foster this growing relationship between the OSU campus and the greater Corvallis Community. Go Beavers!


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Local & family history, nostalgia
Family history, tracing ancestors
The Secret Life of Dorothy Soames	Losing and Finding My Mother in the Foundling Hospital
Justine Cowan (author)
Hardback (04 Feb 2021)
Hardback (12 Jan 2021) $38.21 $25.12
A gripping memoir and revelatory investigation into the history of the Foundling Hospital and one girl who grew up in its care - the author's own mother.
'Page-turning and profoundly moving' VIRGINIA NICHOLSON
Growing up in a wealthy enclave outside San Francisco, Justine Cowan's life seems idyllic. But her mother's unpredictable temper drives Justine from home the moment she is old enough to escape. It is only after her mother dies that she finds herself pulling at the threads of a story half-told - her mother's upbringing in London's Foundling Hospital. Haunted by this secret history, Justine travels across the sea and deep into the past to discover the girl her mother once was.
Here, with the vividness of a true storyteller, she pieces together her mother's childhood alongside the history of the Foundling Hospital: from its idealistic beginnings in the eighteenth century, how it influenced some of England's greatest creative minds - from Handel to Dickens, its shocking approach to childcare and how it survived the Blitz only to close after the Second World War.
This was the environment that shaped a young girl then known as Dorothy Soames, who was left behind by a mother forced by stigma and shame to give up her child; who withstood years of physical and emotional abuse, dreaming of
escape as German bombers circled the skies, unaware all along that her own mother was fighting to get her back.
'A gripping true story' Christina Baker Kline, bestselling author of ORPHAN TRAIN
'Breathtaking' Adrienne Brodeur, bestselling author of WILD GAME
Imprint: Virago
Pub date: 04 Feb 2021
DEWEY: 362.732
Weight: -1g
The House by the Lake
Thomas Harding (auth...
Published 02 Jun 2016
Tracing Your Air Force Ancestors
Phil Tomaselli (auth...
Published 28 Feb 2014
Renia's Diary
Renia Spiegel, Anna ...
One Two Three Four
Craig Brown (author)
The Secret Life of the Savoy
Olivia Williams (aut...
Anne Glenconner (aut...
The Volunteer
Jack Fairweather (au...
The Lost Homestead
Marina Wheeler (auth...
King and Emperor
Janet L. Nelson (aut...


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A 'Big Brother'-Themed...
Amazing Race, Big Brother, Video-a-Polooza
A 'Big Brother'-Themed Season of 'The Amazing Race' Is Reportedly In The Works
May 7, 2018 by The Ashley
They're going to need to come up with a different hashtag…
CBS was reportedly so inspired by Big Brother's Jessica Graf and Cody Nickson winning The Amazing Race Season 30 that the network is planning to up the 'Big Brother' factor for Season 31!
TMZ reports that CBS is attempting to put together a 'Big Brother'-themed season of 'The Amazing Race' that will feature a cast made up of former 'Big Brother' contestants and winners.
"[CBS] has locked down its list of competitors for the new season, which will begin filming soon," TMZ reported.
The network has already secured one 'Big Brother' winner to compete on 'The Amazing Race' (although TMZ did not specify which winner). Several of the most-popular 'Big Brother' winners declined to participate for various reasons, but the network was still able to secure a decent 'Big Brother'-themed cast.
"CBS is happy with the final cast … and they're ready to race around the world," TMZ stated.
Despite their big win, Jessica and Cody won't be doing another lap around the world on the next season. The couple recently got engaged and are planning their wedding.
Cody and Jessica were not the first 'Big Brother' couple to do 'The Amazing Race.' 'Big Brother' Season 13 winner Rachel Reilly and her now-husband Brendon Villegas did two stints on the show, and 'Big Brother 11' winner Jordan Lloyd and her husband Jeff Schroeder appeared on 'The Amazing Race' Season 16. However, Jordan is currently pregnant), so it's unlikely she and Jeff will appear on 'The Amazing Race' any time soon.
UPDATE! TMZ reports that Caleb Reynolds (aka "The Beast Mode Cowboy" from Season 16) and Rachel have signed on to compete on the new season of 'The Amazing Race.' (There's no word yet if Rachel's husband Brendon will compete as well.)
Relive Jessica and Cody's best moments from 'The Amazing Race' by watching the video below!
(Photo: CBS)
Tags: Amazing Race, Big Brother, Big Brother 19, Big Brother Cast, Cody Nickson, Jessica Graf, The Amazing Race Season 31, Videos
Depending on the couples, I would watch! But don't bring on awful people (like Mark and Elena) just for the sake of it being BB themed!
meech says:
for the love of god please do not let it be elena and mark
Dolly says:
Hell yeah ???


The hexadecimal color code #19391a is a dark shade of green. In the RGB color model #19391a is comprised of 9.8% red, 22.35% green and 10.2% blue. In the HSL color space #19391a has a hue of 122° (degrees), 39% saturation and 16% lightness. This color has an approximate wavelength of 548.43 nm.


Summary: Wireless backhaul networks have recently seen a shift towards packet switching, wherein data is transmitted and routed independently in segments known as packets. This change has been necessitated by the growing demand on backhaul networks to support increased data rates. However, in packet switched networks, packets take random amounts of time to travel between their source and destination, a problem referred to as packet delay variation (PDV). PDV is undesirable since it hampers accurate time synchronization over backhaul networks. While several techniques to combat PDV in the context of synchronization have been developed, they often fail to perform effectively under stressful network conditions. The proposed research aims to extend work done under an ongoing PITA grant, where the nature of PDV was studied under many different network conditions, and new theoretical limits on the performance of techniques that combat PDV were obtained. The extension of this work will involve the development of new schemes that improve performance over existing schemes to combat PDV, while also being able to adapt to changing network conditions. The efficiency of the proposed schemes will be studied via simulations and their implementations will be optimized for ARM processors. The project is collaboration between the Lehigh team and the System Architecture Group at the LSI facilities in Allentown, PA. LSI is an electronics company that develops network technology.


The specifications of your electronic and electrical connectors are very precise. Even the tiniest discrepancy in size, weight, or material used can make your product less efficient and unmarketable. When you are designing and producing your electronics and electrical connectors, make sure you work with a company that specializes in electronic plastic injection molding. Superior Plastics has the expertise and equipment that you need to produce quality electronics and electrical connectors. We are a plastic injection molding company you can trust as your electronic connector supplier.
The high-performance plastic injection molding machines we use at Superior Plastics give you the most versatile options for your electronics and electrical connectors. Our connector plastic injection molding makes it possible to make products specific to you, our client. The great advantage this has is that it gives you more options for your design. You can create your own plastic electronic and electrical connectors that fit right where you need them.
Having the ability to specify the design of your electronics and connectors by using electronic plastic injection molding is also economical. You can design a part that has the exact specifications you need for your product. Why pay for several generic pieces, if one custom piece that has the same function will do? Simplify your product and save money on production. With injection molding from the manufacturer, you get exactly what you need.
At Superior Plastics, we have worked with many different businesses in several industries to supply their electronics and electrical connectors. We are capable of handling plugs and plug-ins for office equipment, medical equipment, robotics, and heavy machinery. We have worked with clients in the military, telecommunications, and automotive industries.
Connectors and electronics need to be very precise. Our experience in producing electronics and connectors is a great benefit to you. We know what it takes to get a quality product at a reasonable price. We can help you with the material, design, and specifications you need. Whether you are working on a prototype or looking to mass produce, Superior Plastics can meet your needs.
As with all of our services, the personal touch we give at Superior Plastics is second to none. If you have more questions about our services in electronic and electrical connector plastic injection molding, contact us at 817-882-9595. We would love to talk with you about your electronic connector plastic injection Molding needs today.


Why Brand Modi needs to be Team Modi in order to win?
Narendra Bhai Modi has already started his campaign towards 7, RCR. He has lead Gujarat with a confidence rarely seen on the Indian political canvas. Excellent Orator, a macho image and a development czar almost in the mold of the initial years of Lee Kuan Yew, all make him a hit ticket entity for the … More Why Brand Modi needs to be Team Modi in order to win?
2 Comments Why Brand Modi needs to be Team Modi in order to win?


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To be fair, in my case, it wasn't too excruciating. My high school had a rather reasonable start time of 8:10; moreover, since I lived close to my school, I could usually get away with waking up after 7:00 a.m. Others I spoke to were not so fortunate; the combination of pre-8 a.m. start times, combined with long bus rides, required them to wake up well before 6 a.m. Looking at the data, this isn't all that unusual. 40 percent of public schools start before 8 a.m., according to an article in Scientific American. Factor in long bus rides and it becomes clear why 75 percent of teenagers get fewer than 8 hours of sleep on school nights, per a 2015 survey from the Center for Disease Control.
The combination of early school hours and an adolescent sleep schedule makes for an unsurprising result: Most teenagers aren't getting enough sleep. In 2018, the American Academy of Sleep Medicine recommended all middle and high schools start after 8:30 a.m.; this is a goal that currently only 17 percent of public schools achieve, according to the CDC. While experts recommend teens get 8-10 hours a night, only 15 percent of teenagers slept at least 8.5f hours on school nights, reports the National Sleep Foundation.
Now, this might all seem a little obvious — "teenagers don't like waking up early" is hardly breaking news. But even more interesting are the repeated studies displaying the many areas where students benefit when they wake up later, per the Washington Post. Some you'd expect: attention span increases and tardiness decreases. But there are other benefits, too — marked improvements in academic performance, mental and physical health, a reduction in teen vehicle accidents, behavioral issues and sleep disorders.
What's more, students from economically disadvantaged backgrounds experienced the biggest drawbacks from early start times. The Hamilton Project at the Brookings Institute found that "early school start times reduce performance among disadvantaged students by an amount equivalent to having a highly ineffective teacher" in a 2011 paper. The science clearly supports one side of this debate, and it's not the side that wants 16-year-olds to wake up at 5:30 a.m.
So — if all these findings are out there, why do high schools still start so early? The reasons are unclear. Two common arguments rest on having adequate time for after-school sports practice and the financial cost of shifting bus schedules. But, per the Washington Post, many districts have overcome the athletics issue "with flexibility on the part of the staff and coaches," and while changing bus schedules can sometimes be costly, "this isn't a certainty" — schools often overestimate the financial burden of these changes.
Another argument is that working parents' schedules may not align with a later start time. But the current system is already inconvenient for them, as traditional school days "usually end a good two hours before the typical American workday does," per a 2018 Atlantic article. And given that high schoolers are both far more autonomous than elementary schoolers, and would benefit more from later start times, shifting the schedules for older students more than for younger ones would minimize disruption to parents' lives.
A more general reason: School systems are vast, complex entities that are slow to implement change. After all, as the Atlantic reports, many of our traditional school vacations originate in agricultural family's need to have their children home to help out during harvest time. School schedules are rooted in past traditions, and large-scale changes can be daunting, especially when making a mistake has the potential to affect so many people.
I believe there's also a lack of action on this issue because of the attitude society has toward adolescents in general, and specifically beliefs surrounding teenage laziness and the character-building experience of rolling out of bed semi-conscious. As a society, we should try to base our policy-making on logic, rather than vague notions of the "benefits" of early rising.
On this front, there's some good news — in recent years, some schools have decided to act. "Hundreds of schools in 44 states have jumped on the late-start bandwagon" in response to advocacy groups, per a 2017 Business Insider article. In fact, my district was one of them. My older sister remembers classes starting at 7:40, before start times were pushed back that precious half hour. Hopefully, this growing body of research will be enough to convince administrators to give the issue a closer look. Until then, one thing is clear: we should all be thankful for our 9 a.m. classes.