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John Harvey KelloggM. February 26, — December 14, was an American medical doctor, nutritionist, inventor, health activist, and businessman.
The sanitarium was founded by members of the Seventh-day Adventist Church. It combined aspects of Ladies wants hot sex Orono European spa, a hydrotherapy institution, a hospital and a high-class hotel. Kellogg treated both the Kitchener ontario swingers and famous and the poor who could not afford other hospitals.
Disagreements with other members of the church led to a major schism within the denomination: Ladies wants hot sex Orono was disfellowshipped inbut continued to follow many Adventist beliefs and directed the sanitarium until his death in Kellogg also helped to establish the American Medical Missionary College in The College operated independently untilwhen it merged with Illinois State University.
Kellogg was a major leader in progressive health reform, particularly in the second phase of the clean living movement. His approach to "biologic living" combined scientific knowledge with Adventist beliefs, promoting health reform, temperance and sexual abstinence.
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His promotion of developing anaphrodisic foods were based Oronno these beliefs. Many of the vegetarian foods that Kellogg developed and offered his patients were publicly marketed: Kellogg is best known today for the invention of the breakfast cereal corn flakesoriginally intended to be an anaphrodisiac, [3] with his brother, Will Keith Kellogg.
Kellogg was an early proponent of the new germ theory of diseaseand well ahead of his time in relating intestinal flora and the presence of bacteria in the intestines to health and disease. The sanitarium approached treatment in a holistic manner, actively promoting vegetarianism, nutrition, the use of enemas to clear intestinal flora, exercise, sun-bathing, hydrotherapyand abstention from OOrono tobacco, drinking alcoholic beverages hpt sexual activity.
John Preston Kellogg became a member of several revivalist movements, including the Baptiststhe Congregationalist Churchand finally the Seventh-day Adventist Church. White and her husband James Springer White to relocate Ladies wants hot sex Orono Battle Creek, Michiganwith their publishing business, in There John Preston Kellogg established a broom factory. The Kelloggs believed that the Second Coming of Christ was imminent, and that formal education of their children was therefore unnecessary.
Originally a sickly child, Women seeking nsa Clyde Hill Harvey Kellogg attended Battle Creek public schools only briefly, from ages 9— He left school to work sorting Ladies wants hot sex Orono in his father's broom factory.
Nonetheless, he read voraciously and acquired a broad but largely self-taught education. At age 12, John Harvey Kellogg was offered work by the Whites.
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White's theories of health, and beginning to follow recommendations such as a vegetarian diet. OOrono hoped to become a Ladies wants hot sex Orono, and at age 16 taught a district school in Hastings, Michigan.
He graduated in with a medical degree. Kellogg followed Adventist views in favor of celibacy.
The couple maintained separate bedrooms and did not have any biological children. However, they were foster parents to 42 children, legally adopting at least seven Bulawayo Hartford girls them, before Ladies wants hot sex Orono died in Pulitzer Prize historian Will Durantwho had been a vegetarian wanhs the age of 18, called Dr. Kellogg "his old mentor", [18] and said that Dr.
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Kellogg, more than any Ladiws person since his high school days, had influenced his life. Kellogg died on December 14,in Battle Creek, Michigan. Kellogghis brother's wife, James WhiteEllen G. PostUriah Smithand Sojourner Truth. Kellogg was brought up in the Seventh-day Adventist Church from childhood, at a time when members commonly engaged in theological speculation.
Throughout his lifetime, Kellogg experienced pressure from both science and religion regarding his theological views. This resolution was unanimously adopted, after Hot sexy women Bartlesville Oklahoma the Oroono adjourned to the call of the chair. Kellogg gave, before a large audience, October 6, an able address on wqnts harmony of science and the Bible, Ogono which the congregation tendered him a vote of thanks.
Kellogg attempted to defend "the harmony of science and the Bible" throughout Ladies wants hot sex Orono career, but he was active at Ladies wants hot sex Orono transitional time, when both science and medicine were becoming increasingly Ladies wants hot sex Orono. White and others in the Adventist ministry worried that Kellogg's students and staff were in danger of losing their religious beliefs, while Kellogg felt that Sex women va man fuck family Newdale Idaho ID ministers failed to recognize his expertise and the importance of his medical work.
There were ongoing tensions between his authority as a doctor, and their authority Mature women 29906 ministers.
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The heart is a muscle. My arm will contract and cause the fist to beat; but it beats only when my will commands. But here is a muscle in the body that beats when I am asleep.
It beats when my will is inactive and I am utterly unconscious. It keeps on beating all the time. What will is it that causes this heart to beat?
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The heart can not beat once without a command. To me it is a most wonderful thing that a man's heart goes on beating. It does not beat by means of my will; for I can not stop bot heart's beating, or make it beat faster or slower by commanding it by my will.
But there is a will that controls the heart. It is the divine will that causes it to beat, and in the beating of that heart that you can feel, as you put your hand upon the breast, or as you put your finger against the pulse, an evidence Laies the divine presence that we have within us, that God is within, that there is an intelligence, a power, a will within, that is commanding the functions of our bodies and controlling them… [24].
There is a clear, complete, satisfactory explanation of the most subtle, the most marvelous phenomena of nature,—namely, an infinite Intelligence working out its purposes. God is the explanation of nature,—not a God outside of nature, but in nature, manifesting himself through and in all the objects, movements, and varied phenomena of the universe. The tree does not create itself; Girl seeking cowboy creative jot is constantly going forward in it.
Buds and leaves come forth from within the tree So there is present in the tree a power which creates Ladies wants hot sex Orono maintains it, a tree-maker in the tree, a flower-maker in the flower,—a divine architect who understands every law of proportion, an infinite artist who possesses a limitless power of expression in color and form; there is, in all the world about us, an infinite, divine, though invisible Presence, to which the unenlightened may be blind, but which is ever declaring itself Online personal check its ceaseless, beneficent activity.
At the same time that Kellogg defended the presence of God in nature against secularization, his co-religionists saw his descriptions of the presence of God in nature as evidence of pantheistic tendencies God is in everything.
What came to be referred to as the "Pantheism Crisis" of was a pivotal moment in the church's history. Kellogg's theological views were only one of the issues involved: Ladies wants hot sex Orono, who had proclaimed Ladies wants hot sex Orono a cleansing sword of fire was poised over the increasingly "worldly" and business-oriented Battle Creek, was against the rebuilding of a large institution.
The new building was designed by architect Frank Mills Andrews of Ohio [31] and opened on May 31, Kellogg used proceeds from his book The Living Temple to help pay the costs of reconstruction. The book's printing was opposed by a commission of the General Council of the Adventists after W.
Prescottone of the four members of the commission, argued that it was Ladies wants hot sex Orono. Jot Kellogg arranged to print it privately, the book went through its own trial by fire: Kellogg retained control of the Battle Creek Sanitarium and the American Medical Missionary College, and continued Otono promote Adventist ideas of Ladies wants hot sex Orono and well-being at those institutions. White's prophetic ministry, despite their struggles.
Facial Rejuvenation Acupuncture Classes How To Prevent Wrinkles On Your Chest Exposed Skin Care Uk Reviews Instant Wrinkle Removers Best Skin Clinic In Milwaukee Anti Aging Drug Approved A total skincare moisturizer would contain plant-based oils and the lot of antioxidants. Identical shoes you wear good foods we eat can be employed directly to boost our skin's health and show off. John Harvey Kellogg, M.D. (February 26, – December 14, ) was an American medical doctor, nutritionist, inventor, health activist, and businessman. He was the director of the Battle Creek Sanitarium in Battle Creek, performance-therapeutics.com sanitarium was founded by members of the Seventh-day Adventist performance-therapeutics.com combined aspects of a European spa, a hydrotherapy institution, a hospital and a. Leicester Skin Clinic Skin Clinic Houston New Age Skin Care Bbb Leicester Skin Clinic L Arginine Anti Aging Benefits Clinique Skin Care Samples Clinique Skin Care Samples When I made the switch from normal anti aging lotions to natural ones I noticed an immediate difference, harmful. " just a small one. These decisions ought not to be made lightly and if you have had trouble finding an.
Inin response to critic E. Ballenger, Kellogg admonished Ballenger for his critical attitude to Mrs. White was unquestionably an inspired woman. In spite of this fact, she was human and made many mistakes and probably suffered more from those mistakes than any person ever did. Nevertheless, I knew the woman was sincere and honest and that the influence of her Connerville Oklahoma horny milfs some where Randlett Utah nsa and ltr was immensely helpful to a vast multitude of people, and I have not the slightest desire in any way to weaken in the smallest degree the good influence of her life and work.
Kellogg was a Ladies wants hot sex Orono Adventist until mid-life, and gained fame Ladies wants hot sex Orono being the chief medical officer of the Battle Creek Sanitarium, which was owned and operated by the Seventh-day Adventist Ladies wants hot sex Orono. The Sanitarium was operated based on the church's health principles. Adventists believe in promoting a vegetarian diet, abstinence from alcohol and tobacco, and a regimen of exercise, all of which Kellogg followed.
He is remembered as an advocate of vegetarianism [35] and wrote in favor of it, even after leaving the Adventist Church.
His development of a bland diet was driven in part by the Adventist Orino of reducing sexual stimulation. Kellogg was an especially strong proponent of nutswhich he believed would save mankind in the face of Ladies wants hot sex Orono food supplies. The Battle Creek Sanitarium had its own experimental kitchen. There Ella Eaton Kellogg helped to develop vegetarian foods, and supervised a "school of cookery" which taught classes in food preparation for homemakers.
Kellogg believed that most disease is alleviated by a change in intestinal flora ; that bacteria in the Adult wants hot sex Niarada Montana 59852 can either help or wwnts the body; that pathogenic bacteria produce toxins during the digestion of protein that poison the blood; that a poor diet favors harmful bacteria that can then infect other tissues in the body; that the intestinal flora is changed by diet and Ladies wants hot sex Orono generally changed for the better by a well-balanced vegetarian diet favoring low- Ladies wants hot sex Oronolaxativeand high- fiber foods.
He even recommended various regimens of specific Ladjes designed to heal specific ailments. Kellogg further believed that natural changes in intestinal flora could be sped by enemas seeded with favorable bacteria.
He Deltona florida sex. the frequent use of an Laddies machine to cleanse the bowel with several gallons of water. Ladiss enemas were followed by the administration of a pint of yogurt —half was eaten, the other half was administered by enema, "thus planting the protective germs where they are most needed and may render most effective service.
Sanitarium visitors also engaged in breathing exercises and mealtime marches, to promote proper digestion of food throughout the day.
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Because Kellogg was a staunch supporter of phototherapythe sanitarium made use of artificial sunbaths. Kellogg was a skilled surgeon, who often donated his services to indigent patients at his clinic.
John Harvey Kellogg developed and marketed a wide variety of vegetarian foods. Many of them were meant to be suitable for an invalid diet, and were intentionally made easy to chew and to digest.
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Starchy foods such as grains were ground and baked, to promote the conversion of starch Ladifs dextrin.
Nuts were ground and boiled or steamed. The foods Kellogg developed also tended to be bland.
In this, Kellogg followed the teachings of Ellen G. White and Sylvester Graham who recommended a diet of bland foods to minimize excitement, sexual arousal, and masturbation.
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Хра́мова гора́ (,Гар га-Байт, , аль-Харам аль-Кудс аш -Шаріф — «благородне святилище») — пагорб над Кедронською долиною у південно-східній частині старого міста Єрусалима. Храмова гора — обнесена високими стінами прямокутна площа, що виділяється над іншими частинами Старого міста. Висота кам'яної стіни у найвищому місці 45 метрів. Загальний об'єм кам'яної кладки стіни близько двохсот тисяч кубічних метрів - трохи менше об'єму кладки, наприклад, третьої піраміди (піраміди Менкаура) на плато Гіза. Раніше тут стояв Єрусалимський Храм. Зараз на ній розташовані мусульманські святині — Мечеть Аль-Акса (далека мечеть) і Ма́сджид Ку́ббат ас-Са́хра (відома також як Купол Скелі), побудовані Абд аль-Маліком у 691 році. Храмова гора є священним місцем для послідовників юдаїзму  та ісламу.

Історія
Юдеїв, християн та мусульман поєднують з Храмовою горою багато релігійних подій та традицій. За переданнями Талмуду, з цього місця Бог взяв землю для створення Адама. На цьому місці Адам, пізніше Каїн і Авель, Мелхіседек і Ной приносили свої жертви. Храмова гора традиційно ототожнюється з місцевістю Моріа — так називається земля на якій стоїть Храмова гора і на якій Авраам, випробовуваний Господом, мав принести у жертву свого сина Ісаака (). У юдейській, християнській і мусульманській традиціях це те саме місце. На Храмовій горі цар Давид викупив за п'ятдесят шеклів тік у якогось Аравни (євусеянина) () і спорудив жертовник Богу Ізраїлю, а його син і спадкоємець престолу — Соломон побудував там Перший Храм у X столітті до н. е (957 р. до н. е — освячений 951 до н. е.). У 586 році до н. е. Перший Храм був зруйнований Навуходоносором. Після повернення євреїв в Єрусалим з вавилонського полону у 515 році до н. е. був побудований Другий Храм. Цар Ірод під час розпочатої ним реконструкції Храму у 22 році до н. е. збільшив площу Храмової гори, звівши навколо неї потужну підпірну стіну і засипав землею проміжок між стіною і пагорбом. Реконструкція тривала і спадкоємцями Ірода — Агріппою I і Агріппою II аж до Юдейської війни 67 року н. е. Храм Ірода проіснував до 70 року н. е., коли був зруйнований римлянами під проводом Тита. Після цього римляни будують на Храмовій Горі Храм Юпітера і дещо пізніше там було побудовано християнську церкву. Після захоплення арабами Палестини у 638 році на Храмовій Горі вони побудували свої храми.

У ісламі Храмова Гора є третім за значенням місцем після Мекки і Медіни. Сюди здійснив пророк Мухаммед свою нічну поїздку з Заповідної у Найвіддаленішу мечеть (мечеть аль-Акса)(сура 17. вірш 1).  Сьогодні на Храмовій горі розташовані дві ісламські святині, присвячені цій події — мечеть аль-Акса, що означає найдальша, та Купол Скелі, зведений над Каменем заснування, з якого Магомет здійнявся в небо.

Третій храм
Докладніше
Ідея відновлення Третього Храму на Храмовій горі в Старому місті залишається ключовим предметом напруженості між мусульманами та євреями через існування Куполу Скелі, ісламське святилище, побудоване на місці першого та другого єврейських храмів під час правління Омейядів наприкінці 7 століття.

Новітня історія
У періоди правління Палестиною арабів, османів і британців, євреї не допускалися на Храмову гору. Британська мандатна адміністрація ввела спеціальний орган по опіці над святими місцями ісламу на Храмовій горі — ВАКФ, чи Ісламська рада (Muslim Council), орган який отримав фактичну владу над усією територією Храмової гори. Після закінчення Війни за незалежність Ізраїлю у 1948 році, Храмова гора разом з усім Східним Єрусалимом перейшла під контроль Йорданії. До 1967 року євреї не допускалися не тільки на Храмову гору, але й до Стіни Плачу. Під час Шестиденної війни, в ході боїв за Єрусалим, ізраїльські десантники встановили контроль над Храмовою горою. Однак незабаром, за наказом міністра оборони Моше Даяна, ізраїльський прапор було спущено, і повноваження Ісламської ради щодо Храмової гори знову були офіційно підтверджені. З 1967 року на Храмову гору був відкритий доступ усім охочим у відведені дні й години.

Доступ до Храмової гори
Доступ до Храмової гори можливий через одинадцять воріт із північної та східної сторін. Всі ворота охороняються поліцією Ізраїлю та співробітниками ВАКФ, оскільки доступ до Храмової гори через 10 воріт дозволений лише для мусульман. Представникам іншої віри можливий доступ лише через Марокканські ворота. Прохід дозволений лише у часи між молитвою та з суботи до четверга. Не дозволено приносити з собою культові речі, затримуватися для молитви не-мусульманам.

Теракти
У січні та липні 2017 року на Храмовій горі сталось декілька терактів, що привели до загибелі семи правоохоронців та чотирьох терористів.

Галерея

Панорама

Примітки

Посилання

 Єрусалимські Храми в Ісламі

Біблійні місця
Єврейська історія
Новий Заповіт
Старий Заповіт
Культові споруди Єрусалима
Історія юдаїзму
Гори Єрусалима
Священні гори

redpajama_set_name: RedPajamaWikipedia


text:
\section{Introduction}
The leading explanation for the delivery of water to Earth is that water-bearing, asteroid-like bodies from beyond the snow line were gravitationally scattered inward and accreted by the planet during its growth \citep[e.g.][]{Morbidelli:2000ex}.
If the same mechanism also operates in extra-solar planetary systems, the water content of potentially habitable terrestrial planets that formed in situ depends on both the snow line location and the extent to which water-bearing materials were scattered inwards. For lower-mass M dwarf stars, N-body simulations indicated that terrestrial planets in the habitable zone would be dry \citep{2007ApJ...669..606R, 2007ApJ...660L.149L}, in contrast to planets that formed farther out in the disk and migrated to their current locations \citep{Ogihara:2009cu}. In a previous paper \citep{Ciesla:2015ha}, we explored how the inclusion of planetesimals and more comet-like bodies in these simulations can enhance volatile delivery around these low-mass stars. In that work, the location of the snow line was a critical factor in determining how much water would be delivered to forming planets.  Here, we revisit the location of the snow line based on recent protoplanetary disk observations, and explore its impact on water delivery to habitable zone terrestrial planets.

\begin{figure*}
	\includegraphics[width=0.7\linewidth]{fig1a.pdf}
	\includegraphics[width=0.7\linewidth]{fig1b.pdf}

	\caption{Location of the snow line for a range of stellar masses for a disk of small ISM-like grains (top\xspace panel) and larger grains more representative of protoplanetary disks (bottom\xspace). The green/red line, dark-shaded area and light-shaded area show the median, $\pm 1\sigma$, and $\pm 2 \sigma$ location of the snow line, respectively, calculated from the observed distribution of mass accretion rates using Eq. \ref{eq:analytical}.
	\label{fig:diag}
	}
\end{figure*}

In the Solar System, the location of the snow line at the time of planetesimal formation has been inferred from the transition between hydrous and anhydrous asteroids to be $\sim 2.5$ au \citep{Abe:2000vr}. There is, however, a considerable uncertainty in this location if asteroids have been scattered into their current locations \citep[e.g.][]{2012M&PS...47.1941W,DeMeo:2014hk}.
There are no direct measurements of the location of a water snow line outside our solar system, hence we do not know if it is typical for sun-like stars. The Solar System snow line location of 2.5 au has been taken as a reference point in previous studies, and used to estimate the location around other stars of various masses \citep[e.g.][]{2007ApJ...669..606R}. The exact location of the snow line will be determined by the combined irradiative and viscous heating in the disk \citep[e.g.][]{Davis:2005ho}.  If mass accretion occurs through the vertical extent of the disk, the mid plane temperatures at the relevant locations are set by the release of gravitational potential energy for mass accretion rates $>10^{-10} \ensuremath{M_\odot / {\rm yr}}\xspace$, and the location of the snow line is a strong function of mass accretion rate \citep{2007ApJ...654..606G,Oka:2011jh}.

The dependence of mass accretion rate on stellar mass has been well-established, following a roughly quadratic relationship \citep[e.g.][]{Muzerolle:2003ha,2004AJ....128.1294C,2005ApJ...625..906M, 2006A&A...452..245N}, but these relations have not been used to calculate the location of the snow line around low-mass stars. On top of that, there is an intrinsic dispersion in mass accretion rates of $\sim 0.4$ dex around this relation \citep{2014A&A...561A...2A}. If this intrinsic dispersions reflects a range in initial disk masses, which is of the same order, 0.5 dex \citep{Armitage:2003dc}, we expect an associated dispersion in snow line locations (Figure \ref{fig:diag}), leading to enhanced or reduced water delivery among stars of similar mass.

In addition to the mass accretion rate, the location of the snow line in a protoplanetary disk around a sun-like star is very sensitive to the dust opacity \citep{2011Icar..212..416M, Oka:2011jh}.  While previous work on the snow line location in the solar nebula had mainly used small sub-micron sized grains \citep[e.g.][]{Davis:2005ho,2007ApJ...654..606G}, there is abundant observational and theoretical evidence that grains in protoplanetary disks quickly grow to millimeter and centimeter sizes \citep[e.g.][]{2014prpl.conf..339T}, depleting the amount of small grain by orders of magnitude \citep[e.g.][]{2006ApJS..165..568F}. Lower dust opacities trap viscous heat less efficiently, resulting in a cooler disk mid plane with a snow line closer to the star, enhancing water delivery.

In this work, we explore the range of snow line locations that may be expected for stars of different masses, factoring in variations in disk mass accretion rate and dust opacities that have been inferred for real disks (\S \ref{sec:SL}) and how
this would impact the water content of terrestrial planets in the Habitable zone (\S \ref{sec:nbody}).

\begin{table*}

	\centering

	\begin{tabular}{l l l l l l}\hline\hline
	$M_*$ 			& $\log \dot{M}$  		& \multicolumn{2}{c}{\ensuremath{R_{\rm SL}}\xspace (1-$\sigma$)} & \multicolumn{2}{c}{\ensuremath{R_{\rm SL}}\xspace} \\
	 				& 						& small grains 	& large grains & MS & pre-MS \\
	{}[$M_\odot $]	& [$\log M_\odot /{\rm yr}$]		& [au] & [au] & [au] & [au] \\
	\hline
	$1.0$ & $-7.5 \pm 0.4$ & $3.3$ ($2.2$...$5.0$) & $1.6$ ($1.1$...$2.4$) & 2.5 & 1.35 \\
	$0.8$ & $-7.7 \pm 0.4$ & $2.6$ ($1.7$...$3.9$) & $1.2$ ($0.82$...$1.9$) & 1.23 & 1.15 \\
	$0.6$ & $-7.9 \pm 0.4$ & $1.9$ ($1.2$...$2.8$) & $0.9$ ($0.59$...$1.3$) & 0.61 & 0.95 \\
	$0.4$ & $-8.3 \pm 0.4$ & $1.2$ ($0.78$...$1.8$) & $0.6$ ($0.37$...$0.84$) & 0.32 & 0.8 \\
	$0.2$ & $-8.8 \pm 0.4$ & $0.5$ ($0.36$...$0.81$) & $0.2$ ($0.17$...$0.38$) & 0.16 & 0.5 \\

	\hline\hline\end{tabular}
	\caption{
	Mass accretion rates and location of the viscous snow line as a function of stellar mass used in this work, including one-sigma ranges. For comparison, the last two column shows the snow line locations calculated from the stellar luminosity used in previous work: MS (main-sequence, \citealt{2007ApJ...669..606R}) and pre-MS \citep{Ciesla:2015ha}.
	}
	\label{tab:SL}
\end{table*}

\section{Snow line location in a viscous disk}\label{sec:SL}

The location of the snow line, \ensuremath{R_{\rm SL}}\xspace, in a steady-state viscous protoplanetary disk, assuming it is optically thick to its own radiation, is given by \cite{2011Icar..212..416M}, their Eq. (11):
\begin{equation}
	\label{eq:analytical}
	\ensuremath{R_{\rm SL}}\xspace =  \left(\frac{3 \mu m_p (GM_\star)^{3/2}\dot{M}^2\kappa_R}{128 \pi^2 k_b \sigma_{\rm SB} T_{\rm ice} f \alpha}\right)^{2/9},
\end{equation}
where $\mu$ is the mean molecular weight, $m_p$ the proton mass, $G$ the gravitational constant, $\dot{M}$ the mass accretion rate, $M_\star$ the stellar mass, $\kappa_R$ the Rosseland mean opacity, $k_b$ the Boltzmann constant, $\sigma_{\rm SB}$ the Stefan-Boltzmann constant, $T_{\rm ice}$ the temperature where water ice condenses, $f$ the gas-to-dust ratio, and $\alpha$ the turbulent mixing strength. This equation is based on the estimate of the mid plane temperature of a viscous disk by \cite{Hubeny:1990kr}. \cite{2011Icar..212..416M} showed that this equation is in good agreement with the snow line computed through detailed radiative transfer modeling for a sun-like star. Even though the role of irradiation becomes larger when using the pre-main sequence luminosity and when considering lower mass disks around lower mass stars, we have verified in Appendix \ref{app:mcmax} that viscous heating indeed dominates the thermal budget of the disk mid plane for the range of stellar masses and disk mass accretion rates explored in this paper.

The ice sublimation temperature is thought to lie between 150 and 170 K \citep[e.g.][]{Podolak:2004er}, depending on the water vapor pressure in the disk. The radiative transfer models in \cite{2011Icar..212..416M} include a detailed treatment of solid sublimation as described in \citep{2009A&A...506.1199K}. \cite{2011Icar..212..416M} show that, for a large range of mass accretion rates ---  and hence surface densities and partial vapor pressures --- the location of the snow line is well predicted by assuming a single sublimation temperature of $T_{\rm ice}=160 K$. We therefore do not solve the radial diffusion equation \citep[e.g.][]{2006Icar..181..178C}, as we expect the variations of the partial water pressure by inward drift of evaporating ices to be within the tested range and not lead to large variations in the location of the snow line.

Grouping all constants together, taking $\mu=2.3$, we obtain the more manageable expression
\begin{equation}\label{eq:SLau}
\begin{split}
	\ensuremath{R_{\rm SL}}\xspace= 2.1 ~{\rm au}~ & \left(\frac{M_\star}{M_\odot}\right)^{1/3}
	\left(\frac{\dot{M}}{10^{-8} \ensuremath{M_\odot / {\rm yr}}\xspace}\right)^{4/9}  \\
	& \left(\frac{\kappa_R}{770 ~{\rm cm}^2/g}\right)^{2/9}
	\left(\frac{f}{100}\right)^{-2/9} \\
	&\left(\frac{\alpha}{0.01}\right)^{-2/9}
	\left(\frac{T_{\rm ice}}{160 ~K}\right)^{-10/9}.
\end{split}
\end{equation}
In the remainder of the section we explain the origin and applicability of the parameters in equation \ref{eq:SLau} that lead to the range of snow lines shown in Figure \ref{fig:diag}.

\subsection{Disk mass accretion rate}
The mass accretion rate scales roughly with stellar mass squared \citep[e.g.][]{Muzerolle:2003ha,2004AJ....128.1294C,2005ApJ...625..906M, 2006A&A...452..245N}, with an observed dispersion of up to an order of magnitude around this relation. We will use the observed mass accretion rates from \cite{2014A&A...561A...2A} since these have the smallest observed dispersion, and we will explain in section \ref{sec:spread} how we treat this dispersion.

The \textit{median} mass accretion rate for the $\sim 3 \pm 1$ Myr old \citep{2008hsf2.book..295C} Lupus star forming region, over a range of stellar masses from $0.03~M_\odot$ to $1.0 M_\odot$, is given by \cite{2014A&A...561A...2A}:
\begin{equation}
	\label{eq:alcala}
	\dot{M}_{\rm Lupus}(M_\star) = 5.6 \cdot 10^{-9} \left[\frac{M_\star}{M_\odot}\right]^{1.81} ~\ensuremath{M_\odot / {\rm yr}}\xspace.
\end{equation}

We derive a generic expression for the median mass accretion rate as a function of time by appending this equation with a factor $t^{-3/2}$ to take into account the age of the cluster:
\begin{equation}
	\label{eq:Mdotmedian}
	\ensuremath{\dot{M}_m}\xspace(M_\star,t) = 3 \cdot 10^{-8} \left[\frac{M_\star}{M_\odot}\right]^{1.81} \left[\frac{t}{\ensuremath{\rm Myr}\xspace}\right]^{-3/2} ~\ensuremath{M_\odot / {\rm yr}}\xspace.
\end{equation}
This accretion rate is consistent with the derived accretion rate for the 1 Myr old Taurus region of $\sim 10^{-8} \ensuremath{M_\odot / {\rm yr}}\xspace$ for $\sim 0.5 ~M_\odot$ stars \citep{1998ApJ...495..385H}, and matches well with the observed decay of the mass accretion rate between 0.3 and 30 Myr \citep[][their Figure 2]{SiciliaAguilar:2010jn}. The exponent of $\eta=1.5$ comes from a viscously evolving disk with fixed temperature \citep{2006ApJ...648..484H}, and matches well with the analytical model of \cite{2009ApJ...705.1206C} that includes a changing disk temperature ($\eta=20/13=1.54$) which is more similar to the steady state accretion disk models employed in deriving Eq. \ref{eq:analytical} by \cite{2011Icar..212..416M}. Eq. \ref{eq:Mdotmedian} is only valid at time scales much longer than the viscous time scale, and starts significantly over-predicting the mass accretion rate at $t<0.3$ Myr for $\alpha=0.01$ compared to the \cite{2009ApJ...705.1206C} disk model.

\subsection{Range of snow line locations}\label{sec:spread}
A dispersion in disk mass accretion rate at a given age will lead to a dispersion in snow line locations. Observed mass accretion rates show a large dispersion at any given stellar mass. Part of this dispersion may be attributed to variations in the accretion flow onto the star \citep{2012MNRAS.427.1344C}, and use of secondary tracers of accretion such as emission lines \citep{2012A&A...548A..56R}. An intrinsic dispersion may reflect an age spread and variations in the initial disk mass \citep[e.g.][]{1998ApJ...495..385H}. The tightest constraint on the intrinsic dispersion currently comes from \cite{2014A&A...561A...2A}. Using the X-shooter spectrograph, the authors compute the mass accretion rates using the UV excess emission, a direct tracer of accretion, in the Lupus star forming region over a range of stellar masses from $0.03~M_\odot$ to $1.0 M_\odot$. The dispersion in mass accretion rates \textit{at a given stellar mass} is characterized by a log-normal distribution with a standard deviation $\sigma_{\dot{M}} = 0.4$ dex, a factor of two lower than in previous works. We assume this dispersion reflects a range of initial disk masses as proposed by \cite{1998ApJ...495..385H}.

This assumption is supported by two results. First, the diversity in protoplanetary disk properties, in particular the outer radius-disk mass relation \citep{Andrews:2010eg} and the exponential decay of the disk fraction versus time \citep[e.g.][]{Mamajek:2009de} argue for an intrinsic spread in initial disk masses. Since the inferred spread in disk masses from the time-dependent disks fraction is of the same order, $\sim 0.5$ dex \citep{Armitage:2003dc}, we take the observed dispersion in mass accretion rate to be the intrinsic one. Second, although accretion rates measured from spectral lines are known to be variable on time scales of days to years, this variation is smaller than the observed dispersion and driven by the rotational modulation of the accretion flow onto the star \citep{2014MNRAS.440.3444C}, and does not reflect an intrinsic variation in the \textit{disk} mass accretion rate. It is possible that disks show larger variations at time scales of decades or longer but smaller in magnitude than FUor outbursts, or that it reflect a large age spread in the Lupus cloud, in which case the intrinsic scatter could be smaller.

With the assumption that the observed spread in mass accretion rates is the intrinsic one, the probability distribution of the snow line $R$ around the median, \ensuremath{R_{\rm SL}}\xspace (Eq. \ref{eq:SLau}), is given by a log-normal distribution:
\begin{equation}
	\label{eq:lognormal}
	f_{\rm SL}(R,\ensuremath{R_{\rm SL}}\xspace)= \frac{1}{\sqrt{2 \pi} ~R ~\sigma_R } \exp\left(-\frac{(\log R - \log \ensuremath{R_{\rm SL}}\xspace)^2}{2 \sigma_R^2}   \right)
\end{equation}
with a standard deviation $\sigma_R= 4/9* \sigma_{\dot{M}} \approx 0.18$ dex. This distribution is shown as the shaded regions in Fig. \ref{fig:diag}.

\subsection{Dust opacity}
Since a major source of uncertainty in the calculated location of the snow line is the dust opacity \citep{2011Icar..212..416M}, we explore two limiting cases: the first is where the grains are ISM-like in size as in most previous work, with a Rosseland mean opacity at temperatures relevant for water ice condensation of $\kappa_R = 570 ~{\rm cm}^2/g$, as in \cite{2011Icar..212..416M}; the second is where dust growth is assumed to occur, resulting in a size distribution from micron to centimeter-sized grains, yielding an opacity of $\kappa_R = 20 ~{\rm cm}^2/g$. Such a lower opacity will also increase the amount of solids available for planetesimal formation interior to the snow line, see \cite{2011Icar..212..416M} for details. Because the dependence of the snow line location on this opacity is relatively weak ($\ensuremath{R_{\rm SL}}\xspace \propto \kappa_R^{2/9}$, Eq \ref{eq:SLau}), the snow line moves in by about a factor of two between the two cases considered here (top\xspace and bottom\xspace panels of Fig. \ref{fig:diag}). Table \ref{tab:SL} lists the mass accretion and corresponding snow line locations for the range of stellar masses for the two opacities considered here. Figure \ref{fig:diag} shows the median snow lines for the same stellar mass range, compared to the recent habitable zone estimate from \cite{Kopparapu:2013fu}. Throughout this paper, we use a gas-to-dust ratio $f=66$ based on a condensation sequence at solar metallicity, following \cite{2011Icar..212..416M}.

\subsection{Snow line location}
For a solar mass star with small grains, the one-sigma range of snow line locations encompasses that of the Solar System, from $\sim$2 to $\sim$5 au. Its median location is consistent with the \cite{2009ApJ...705.1206C} disk model for a disk of the same mass accretion rate, age, and opacity. Due to the relatively weak scaling with mass accretion rate ($\dot{M}^{4/9}$), the two-sigma range of snow line location changes by a factor five, even if $\dot{M}$ changes by a factor of $40$.
For the large grain case, the one-sigma locations range from $1.1$ to $2.4$ au, roughly encompassing the habitable zone. In the context of these models, if the solar system snow line was located at 2.5 au at 1 Myr, it is a one-sigma out-lier, and the majority of exoplanetary systems may form with a snow line closer to the star.

Around lower mass stars, the snow line moves closer to the star as $\ensuremath{R_{\rm SL}}\xspace \propto M_\star^{1.14}$ (Eqs \ref{eq:SLau}, \ref{eq:Mdotmedian}). The snow line around a $0.6 M_\odot$ star is closer in compared to that inferred by \cite{2008ApJ...673..502K}, who use a linear scaling of the mass accretion rate with stellar mass which is no longer supported by observations, leading to a hotter disk with a more distant snow line. Compared to the habitable zone, that scales with stellar mass roughly as $R_{\rm HZ} \propto \sqrt{L_{\star, \rm MS}} \propto M_\star^{1.75...2.0}$, the relative gap between snow line and habitable zone widens \citep[See also ][]{2007ApJ...660L.149L}. For the small grain case, the gap between the median snow line and the habitable zone is about a factor of five. For the large grain case, this is only a factor of two, and the two-sigma tail of the snow line distribution overlaps with the habitable zone.

\begin{figure}
	\includegraphics[width=\linewidth]{fig2.pdf}
	\caption{The location of the snow line in au around a solar mass star, for a range of the turbulent mixing strength $\alpha$ and the time $t$ at which the snow line is ``frozen in'' the planetesimal population. Our choice of $\alpha=0.01$ and $t=1$ Myr is shown by the central cross. In general, lower turbulent mixing strength and earlier times move the snow line outward. Towards higher turbulent mixing strength and later times it moves inward.
	\label{fig:timealpha}
	}
\end{figure}

\subsection{Disk viscosity and time of planetesimal formation}
Throughout this paper, we assume $t=1~\ensuremath{\rm Myr}\xspace$ and $\alpha=0.01$ for setting the location of the snow line. Both quantities are not well constrained observationally. The strength of viscosity in protoplanetary disks is inferred to be of order $\alpha \sim 0.01$ based on disk masses, sizes, and lifetimes \citep{1998ApJ...495..385H}. The time that defines the location of the snow line depends on both the planet formation time scale and the extent to which (icy) grains continue to be incorporated into larger bodies as the snow line moves in. The theoretical planetesimal formation time scale at $\sim 1 ~AU$ is of order $0.01-0.1 Myr$ \citep[e.g.][]{Wetherill:1993fp}, and the earliest differentiated bodies formed within $< 1 Myr$ \citep{Kleine:2009jv}, suggesting an early epoch of planetesimal formation. On the other hand, the age of the chondrules in chondritic parent bodies indicate planetesimal formation continued to take place over a 3 Myr time scale \citep[e.g.][]{2014prpl.conf..547J}. If water vapor remains present in the disk, an inward moving snow line may give rise to rapid, but late icy planetesimal formation \citep{2006ApJ...650L.139K}. The age of $t=1~\ensuremath{\rm Myr}\xspace$ is a compromise between two extremes.

To give the reader an idea of how these uncertainties impact the location of the snow line, Figure \ref{fig:timealpha} shows how the location of the snow line varies around a sun-like star with a median mass accretion rate following equation \ref{eq:SLau}. Earlier times and lower turbulent mixing strength correspond to higher surface densities and mass accretion rates that lead to a hotter mid plane and a more distant snow line. Higher mass accretion rates and later times have the opposite effect, leading to a colder, optically thinner disk with a closer-in snow line. In this regime, irradiation may become important as a heating source in the mid plane.

\section{Implications for water delivery}\label{sec:nbody}
To explore how the range in snow line locations may impact the water content of terrestrial planets in the habitable zone, we use the set of N-body simulations from \cite{Ciesla:2015ha}. This approach follows that of \cite{2006Icar..184...39O}, \cite{2007ApJ...669..606R} and \cite{2007ApJ...660L.149L}, for forming terrestrial planets via giant impacts as in the solar system. The simulations are started from a $5 M_\oplus$ disk with equal mass planetary embryos (1/20 Earth mass) and planetesimals (1/20 embryo mass), spaced such that they define a $1/R$ power law in surface density, as in \cite{2006Icar..184...39O}, between 0.5 and 4.0 au. We do not include giant planets, but note that  they may be rare around low-mass stars \citep{Johnson:2010gu} and water delivery can take place in their absence \citep{Quintana:2014hr}. Four simulations are run with near-identical initial conditions to take into account stochastics. These are repeated for lower stellar masses (0.2, 0.4, 0.6 and 0.8 $M_\odot$) by scaling all masses (total, embryo, and planetesimal) to the stellar mass and adjusting the inner and outer edge to encompass both snow line and habitable zone. After 200 Myr, a number of terrestrial planets has formed in the inner regions, see \cite{Ciesla:2015ha} for details.

\begin{figure}
	\includegraphics[width=\linewidth]{fig3.pdf}
	\caption{Planetary water abundances for a $0.6 M_\odot$ star, computed for three different snow line locations (median and $\pm 2 \sigma$). Compare with CC case in figure 6 in \cite{Ciesla:2015ha}.
	\label{fig:ice_SL}
	}
\end{figure}

The water content of these planets depends on the composition of accreted planetary embryos and planetesimals, which in turn depends on their starting locations. We assume that the division between icy and rocky building blocks is located at the snow line, i.e. that planetesimals and embryos do not move radially during their growth process, and that the transition from pebbles to planetesimals and embryos is short compared to the time scale at which the snow line moves inward \citep[e.g.][]{Carrera:2015vy}. Assuming the water content of icy building blocks is low (5\%, similar to carbonaceous chondrites), the extra mass outside of the snow line does not affect the dynamics of the system, allowing the snow line to be inserted \textit{a posteriori}. By keeping track of the starting locations of planetary building blocks that comprise the final planets, their water content can be calculated for different snow line locations from a single simulation. Figure \ref{fig:ice_SL} gives an example of this approach, which shows the water content of planets in the $0.6 ~M_\odot$ simulations calculated from three different locations of the snow line.

\begin{figure*}
	\includegraphics[width=0.7\linewidth]{fig4a.pdf}
	\includegraphics[width=0.7\linewidth]{fig4b.pdf}

	\caption{Fraction of planets in the habitable zone with at least a given mass fraction of water, for stars of different masses. The top\xspace and bottom\xspace panel use a snow line calculated with ISM-like and larger grains, respectively.
	\label{fig:PDF_HZ}
	}
\end{figure*}

By calculating the water content of planets in the habitable zone for a range of snow line locations from the simulations, and assigning to each snow line a probability based on the observed dispersion in mass accretion rates (Eq. \ref{eq:lognormal}, see also Fig. \ref{fig:diag}), we calculate the probability distribution of the water fraction of planets in the habitable zone. These are shown as \textit{cumulative} probability distributions in Fig. \ref{fig:PDF_HZ}.

We take a water mass fraction of 0.1\% as a reference point for early Earth, between 0.03-0.1\% currently in the mantle (\citealt{lecuyer2013water}) and as much as 1\% in the past according to \cite{Abe:2000vr}.
In the simulations with sun-like stars, for a snow line set by small grains, 20\% to 40\% of planets in the habitable zone remain dry, as a fraction of stars has a mass accretion rate high enough to put the snow line too far away from the habitable zone ($~4$-$5$ au) to allow water delivery via giant impacts. The fraction of dry planets is higher in simulations with lower-mass stars, reaching 40\% to 60\% for 0.6 and 0.8 solar mass stars, and close to 100\% for $<0.4$ solar mass stars, in line with previous results (\citealt{2007ApJ...669..606R,Ciesla:2015ha}). The one-sigma range of water fractions spans more than an order of magnitude, significantly larger than the stochastic dispersion in the N-body simulations (a factor of $\sim$2 to $\sim$5).

Using larger grains for calculating the snow line location significantly changes the results. Because the snow line is located closer to the star, water delivery is more efficient: the fraction of dry habitable-zone planets in our simulations decreases to zero for 0.8 and 1.0 solar mass stars, and to 10\% for 0.6 $M_\odot$. A small fraction of habitable zone planets around low-mass stars does receive earthlike amounts of water, around 20\% for 0.2 $M_\odot$ and 0.4 $M_\odot$.

\section{Discussion and Conclusions}\label{sec:discussion}
We derived the fraction of water-bearing terrestrial planets in the habitable zone by assuming they are formed in-situ. There is, however, growing observational evidence that migration of planets or their building blocks plays an important role in the formation of super-Earths and mini-Neptunes at short orbital periods \citep{2012ApJ...751..158H,2013ApJ...764..105S, 2014MNRAS.440L..11R,Mulders:2015ja}. Whether this mechanism  is able to form smaller, earth-sized planets farther out remains an open question. If this were the case, the population of terrestrial planets in the habitable zone might be a mixture of planets formed in-situ and through migration. As migrating planets typically form beyond the snow line \citep[e.g.][]{2014A&A...569A..56C,Izidoro:2014eg}, they are expected to have water mass fractions of order 50\% \citep{Ogihara:2009cu, Tian:2015bx}. Hence, the fractions of wet terrestrial planets quoted in this paper can be considered as lower limits.

An additional concern for the habitability of habitable zone planet around lower mass stars is that water loss may may be more efficient as these planets form hotter than those around sunlike stars \citep{2007ApJ...660L.149L}. \cite{Ramirez:2014bx} show that duing the bright pre-main sequence phase of low-mass stars, stellar fluxes are high enough to trigger a runaway green house effect that leads to enhanced water loss. \cite{Tian:2015bx} come to a similar conclusion by modeling water los through hydrodynamc escape in a planet population synthesis model.
For a planet to remain habitable, water has to arrive later during the pre-main-sequence evolution of the star.
The timing and delivery mechanism of water may be crucial here: In our simulations, water delivery persists over $\sim 100$ Myr time scales. In addition, water is not delivered in the form of ices that would be directly deposited in the atmosphere. Rather, it arrives as hydrated minerals that would enter the atmosphere later via vulcanic outgassing. A detailed study of arrival times and atmospheric release of water may be neccessary to address whether water can be deliverd late enough and in sufficient quantities to avoid escape.

Despite water delivery to low-mass planets in the habitable zone being less efficient than around sunlike stars \citep{2007ApJ...660L.149L,2007ApJ...669..606R}, we show that a small fraction may still receive earthlike amounts of water due to the dispersion in snow line locations. When taking into account the larger number of M stars with respect to G stars (factor ten), their higher planet-occurrence rates (factor two, \citealt{Mulders:2015ja}), and increased water delivery from more comet-like icy bodies \citep{Ciesla:2015ha}, the majority of water-rich terrestrial planets may still be found around low-mass M stars.

\ifemulate
	\ifastroph

redpajama_set_name: RedPajamaArXiv


text:
11 Then Leah said, "Good fortune!" And she called his name Gad.
Genesis 30:11 — The New International Version (NIV)
11 Then Leah said, "What good fortune!" So she named him Gad.
Genesis 30:11 — English Standard Version (ESV)
11 And Leah said, "Good fortune has come!" so she called his name Gad.
Genesis 30:11 — King James Version (KJV 1900)
11 And Leah said, A troop cometh: and she called his name Gad.
Genesis 30:11 — New Living Translation (NLT)
11 Leah named him Gad, for she said, "How fortunate I am!"
Genesis 30:11 — The New King James Version (NKJV)
11 Then Leah said, "A troop comes!" So she called his name Gad.
Genesis 30:11 — New Century Version (NCV)
11 Leah said, "I am lucky," so she named him Gad.
Genesis 30:11 — American Standard Version (ASV 1901)
11 And Leah said, Fortunate! and she called his name Gad.
Genesis 30:11 — 1890 Darby Bible (DARBY)
11 And Leah said, Fortunately! and she called his name Gad.
Genesis 30:11 — GOD'S WORD Translation (GW)
11 Leah said, "I've been lucky!" So she called him Gad [Luck].
Genesis 30:11 — The Holman Christian Standard Bible (HCSB)
11 Then Leah said, "What good fortune!" and she named him Gad.
Genesis 30:11 — The New Revised Standard Version (NRSV)
11 And Leah said, "Good fortune!" so she named him Gad.
Genesis 30:11 — New International Reader's Version (NIrV)
Genesis 30:11 — New American Standard Bible: 1995 Update (NASB95)

redpajama_set_name: RedPajamaCommonCrawl


text:
Diese Liste beschreibt die Mannschaft und die Erfolge des Radsportteams CCC in der Saison 2020.

Erfolge in der UCI WorldTour
In der Saison 2020 gelangen dem Team nachstehende Erfolge in der UCI WorldTour.

Erfolge in den Continental Circuits
In den Rennen des UCI Continental Circuits gelangen dem Team nachstehende Erfolge.

Erfolge in den Nationalen Straßen-Radsportmeisterschaften
In den Rennen der Nationalen Straßen-Radsportmeisterschaften 2020 konnte das Team nachstehende Titel erringen.

Mannschaft

Weblinks

Radsportteam 2020


It was a great day. All the staff that work for Cruise Whitsundays were friendly and approachable. They also kept us informed of what was going on. The trip allowed lots of time to look around at our leisure. They were well equipped at Whitehaven beach, providing water and sunscreen to those who needed it. Was a very enjoyable day. Thanks to all concerned.
Spend a day at Whitehaven Beach and Hamilton Island - two of the Whitsundays and Australia's most famous destinations. Known for its fantastic scenery - crystal clear waters, white sand beaches, and stunning views, there's much to see and do on both destinations. Get to discover all there is to Whitehaven Beach and Hamilton Island with this full day tour. Spend your morning on either Whitehaven Beach or Hamilton Island. Depending on your chosen schedule and package, you can either spend the morning on Whitehaven Beach, or head straight for Hamilton Island. On Whitehaven Beach you can explore the beauty of the entire stretch. Take a dip in the crystal clear waters, go on a self-guided hike to the Hill Inlet lookout, or more! On Hamilton Island, you can opt to take the shuttle bus that'll take you to several destinations on the island, like the swim-up bar in the Main Pool, the long sandy curve of Catseye Beach. Make sure to drop by Front Street, Marina Village for some shopping! After your free time in the morning, enjoy a delicious lunch at the restaurant that goes with your selected package (either Marina Tavern or Manta Ray Cafe), and then head back to the cruise vessel to travel to your next destination, for more free time to explore!
It was a great day. All the staff that work for Cruise Whitsundays were friendly and approachable. They also kept us informed of what was going on. The trip allowed lots of time to look around at our leisure. They were well equipped at Whitehaven beach, providing water and sunscreen to those who needed it. Was a very enjoyable day. Thanks to all concerned. It was a great day. All the staff that work for Cruise Whitsundays were friendly and approachable. They also kept us informed of what was going on. The trip allowed lots of time to look around at our leisure. They were well equipped at Whitehaven beach, providing water and sunscreen to those who needed it. Was a very enjoyable day. Thanks to all concerned.
A good day spent. Many staff onboard and service is good. Don't understand why cruise company has to disallow guests wishing to just stay onboard when in Whitehaven Beach when the boat was just there waiting the whole time. Package lunch at Mantaray is very big in portion despite only a 2 course lunch. Free shuttle bus in Hamilton island is very good. Can circle around island by taking green bus connecting blue bus. A good day spent. Many staff onboard and service is good. Don't understand why cruise company has to disallow guests wishing to just stay onboard when in Whitehaven Beach when the boat was just there waiting the whole time. Package lunch at Mantaray is very big in portion despite only a 2 course lunch. Free shuttle bus in Hamilton island is very good. Can circle around island by taking green bus connecting blue bus.
Beautiful places. Nice weather, Good view! We had a great time. Beautiful places. Nice weather, Good view! We had a great time.
Very good experience!!! Nice and comfortable trip. Very good experience!!! Nice and comfortable trip.


text:
Pelosi Says She Was SET UP to Get Haircut, Demands Apology from Salon At Once
Modified September 2, 2020
House Speaker Nancy Pelosi on Wednesday addressed the controversy surrounding the video of her recent visit to a San Francisco salon, Your Content has learned.
"I take responsibility for trusting the word of a neighborhood salon I've been to over the years many times, and when they said we're able to accommodate people, one person at a time, and that we can set up that time, I trusted that. As it turns out, it was a setup," she said.
The defiant politician added: "This salon owes me an apology."
"It was a set up, and I take responsibility for falling for a setup," she quipped.
She then turned to scold the eSalon owners, demanding they pay her an apology.
And, she threatened, there could be more to the situation than the camera revealed.
"There's more to this that I'm not going to ask to the motivation for a salon to say to me, 'Yes, come in' and then they go for me. It was clearly a set up," she said.


The IAQ Test Kits are to be tested by the consumer.
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Filmatique's Tallinn Black Nights Series concludes with Close Relations, Vitaly Mansky's latest documentary that premiered at Tallinn Black Nights, Toronto, Karlovy Vary and Visions du Réel.
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text:
THE HAGUE, NETHERLANDS - OCTOBER 03: Prinsess Laurentien of The Netherlands, her father Laurens Jan Brinkhorst and her mother Jantien Brinkhorst during the award ceremony of the most influential player in the Dutch philanthropy 2017-2018 organized by De Dikke Blauwe in Societeit de Witte on October 3, 2017 in The Hague, Netherlands. Princess Laurentien is founder of the Missing Chapter foundation that gives children a voice in social issues. (Photo by Patrick van Katwijk/Getty Images)
Getty Images Entertainment Patrick van Katwijk


text:
Monitoring metabolism in real time
Written by Nicholas Miliaras
Biochemistry News
Researchers introduce a device that can continuously measure metabolism, monitor levels of almost any drug, metabolite, or biomarker in the body.
Diagram of the device.
Credit: Netz Arroyo
To achieve the goals of personalized medicine, researchers will need to develop methods for delivering drugs at a time and dose specific to how each patient metabolizes them, which in turn will require a means of precisely and continuously measuring metabolites.
Technologies currently exist for monitoring glucose, lactate, and some neurotransmitters, but these detect only a single molecule as it reacts with a specific enzyme. Now, in the journal PNAS, Kevin Plaxco, Netz Arroyo, and their colleagues at the University of California, Santa Barbara report a device that can measure the levels of drugs, metabolites, and other small molecules in blood.
Plaxco's group used electrochemical sensors (E-AB) coupled to aptamers that can detect a wide range of target molecules. "Our approach seems to be as general as the aptamers are, but you have to change them for each target," noted Plaxco.
Upon binding its target, the apatamer undergoes a conformational change, which changes how a covalently-linked redox reporter transfers electrons to an underlying electrode. The sensor is protected from blood cells by a microporous polysulfone membrane similar to that used in hemodialysis, and it can fit through a 20-gauge needle.
The team implanted their device in jugular veins of anaesthetized rats and tracked real time pharmacokinetics for different antibiotics and chemotherapeutic agents with 3-second temporal resolution. This was sufficient to measure variability in drug metabolism in different rats as well as in the same rat over time. They also obtained precise real-time measurements in rats as they moved about their cages.
Although it could be some time before their device is approved for human use, Plaxco is optimistic. "All the individual components of our device are FDA approved, and it is smaller and lower current than a pacemaker," he said.
Arroyo-Currás N, et al. Real-time measurement of small molecules directly in awake, ambulatory animals. Proc Natl Acad Sci U S A. 2017 Jan 9. pii: 201613458. doi: 10.1073/pnas.1613458114
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text:
Max Anime
Gunnm/Battle Angel Alita
Page 1 of 10 1235 ... Last
Thread: Gunnm/Battle Angel Alita
17 Apr 2005, 06:15 PM #1
MechDeus
Electronic cigarette.
For those who have never read/heard of Battle Angel Alita (Gunnm is the Japanese title - roughly translates as Gun Dream):
It's the story of a scientist that discovers the cyborg head of a girl in a trash heap and reactivates her. Alita (in the Japanese version that's actually the name of his cat, her name was Gally) finds that she can't remember anything about her past but subconciously has access to the Panzer Kunst - an ancient martial art designed by those who lived on Mars specifically to fight robots. She sets off on a quest to find out who she is and where she came from, which (of course) takes her further than she ever expected.
As she tries to find herself she takes up Motorball (a deadly racing sport not unlike Rollerball but on extended Trackmania-esque layouts at incredibly high speeds), music, fighting, and searching for the secret to Salem, the mysterious city in the sky that divides the world by genetic class.
Among what makes this series great is that even with its standard Japanese anime/manga setups it manages to avoid almost all of the tradtional pitfalls; the love stories that occur happen naturally and are not there for comedy, there's almost no SD goofiness or overexaggerated effects, and the science is *gasp* actually well done and thought out (I know, I know; unheard of for Japanese manga writers!). The characters are awesome, they don't pull punches, and the writing is great, weaving together story and explanations so that you're never left in the dark unless he means to but doesn't have an index in the back like Shirow. There's still some, "Haha! You can't beat my attack because it moves like such-and-such!" nonsense here and there but it's not DBZ level or anything.
What few standard weaknesses occur include a little bit of SDism and the ever popular "Tournament time!" that plagues way too many Japanese stories, both of which pop up only during Last Order. On the bright side, the SD is just kinda wierd but never messes with the story (a character gets planted inside a tiny body and is generally totally out of the picture whenever she's not in control of a "real" body), and while the tournament seems way too long considering the pacing of the rest of the series it at least appears to building to an awesome ending.
The progression of the books: Initially Yukito Kishiro made Gunnm from 1990-1995, a series of nine collections in Japan that made it to the states in eight graphic novels (the last two books were combined for the U.S. release). Because of personal and business complications which he has never made public he stopped wanting to make Gunnm about a year before he ended it, but he felt responsibility towards his fans and the story so he forced himself to continue and just kind of threw everything together. Later on he once again wanted to write Gunnm so he expanded the final parts of the story to reach closer to his original ideas and that ended up becoming the expanded story of the PS videogame Gunnm: Martian Memory. After that he once again wanted to truly finish the story so in 2000 he began work on Gunnm: Last Order, a work which was to replace the final book of the original series and give us the true ending. A work which has extended from the singular final book he finished in 1995 into an entire series of seven, of which number five was just released less than a week ago in the U.S. Unfortunately Viz owns the rights to releasing Battle Angel Alita overseas, which means we only get one book every six months and they don't even list the new books or their release dates on their own website. If it wasn't for Amazon I wouldn't even know what date to expect them in stores.
One thing that's interesting to look at is the progression of the art style. In the beginning Alita looked very child-like and the characters often had distinctively stylized faces as is done in many manga, with a lot of the pages meticulously shaded and painted. As it went on it's obvious where time and effort began to take their toll as the art became more simple - still very detailed and beatifully planned out but a lot of the shading was being done less and less. With the break in time between the original series and Last Order it's obvious how far Kishiro has come in his art; all of the characters are drawn in a more cohesive fashion with less reliance on head shape to differentiate them, and the quality of the artwork has increased tremendously. I love the look of LO Alita so much that her original appearance looks wimpy and silly in comparision.
Original Alita Last Order Alita
As at least some of you have read by now, James Cameron is at work on a live-action Alita which will either be his next or after-his-next movie. He's brought up how he wants to focus her character a bit (he felt that her skills went back and forth in terms of strength early on) and also would like to make this a series (he wants Motorball to be in the second movie), so it remains to be seen how things will go. In other offshoots there's an anime of the beginning of the series which I remember being decent but haven't seen in years, and a book called Ashen Victor which focuses on pre-Alita Motorball (which IIRC isn't by Kishiro, but I don't own it and haven't read it).
Obviously I feel this is a fantastic series, if anyone was ever to ask me to recommend a manga it would be hands-down the Alita series. There's nothing else in manga (or comics in general, really) that I think surpasses this, I adored it before and with Last Order it got even better.
elephant.
Yeah, I love this series. Not as much as you, but still quite a bit. I had scattered single issues from when it was first published, and I've collected the books since I noticed it being republished.(Just got 7 & 8 yesterday, actually)
I like Alita's old look much more than the new one though. The new pages are obviously better technically(the art looks a lot cleaner), but I think it loses something there. I can't imagine a design like Figure Four's(was that his name?) showing up in it, for instance, but I liked how that sort of rough design was in Alita. Plus I think she looks better as her wimpy self compared to that Last Order image you chose, anyways. The old contrast of frail body + badass ability thing, I guess. But I've only flipped through the last order books, so my opinion might change once I get used to them.
Ya Skunt
I've been a fan of Alita for quite some time now. It was actually the first anime I'd ever seen outside of the DBZ fare when I was a kid, and when I was in high school I discovered the greatness that was the manga. I finished volume 9 and thought that was the end of it.
But Last Order is just so damned amazing. Kishiro hasn't lost his edge. It has, in fact, gotten far better since his earlier volumes. I must have read volume 4 (the cover of which is on your avatar) at least 8 times now. The fights are just amazing (especially Zazie versus that Kotengu guy) and the continuity and scope are well refined. I do not hesitate to call it the greatest contemporary manga on print right now.
I really hope that Desty Nova comes back at some point, and I also really wonder if we'll ever see Figure Four again. I heartily recommend this to anyone, and if anyone needs the 9 volumes of the first series, there's a certain .zip file I can share with you..
Originally Posted by rezo
The old contrast of frail body + badass ability thing, I guess.
She's still small which I like, but her body seems more developed and he's created more of integration of cybernetics with a human shape. In the old style she was a cyborg that wore clothes and now it's almost as though her armor is just in place of muscle definition (like in my included attachment), which I think is a really cool style. I also think her face is cuter now and I prefer her hair straight instead of the 80's frizz it used to have going on.
Originally Posted by TrialSword
The fights are just amazing
As much as I don't like tournaments, LO4 and 5 have been freaking awesome in the fight department. The last few pages of 5 was just DAMN.
Originally Posted by MechDeus
Five is out now? Hot damn, I need to get this. I was at Kinokuniya in Manhattan a few months ago --they had up to Last Order volume 6 already, and they're bigger and hardcover to boot! Lucky japs get everything...
The cover of volume 6 has Alita/Gally squatting on top of this big purple mass in outer space, with two arm-blades coming from her forearms a la LO volume 4. It's pretty bad-ass. Oh yeah, a calendar pic from Kishiro's site:
EDIT: Kinda funny how they give Figure Four such a prominent spot, and he's been in all of one volume. I mean shit, Kaos has had more impact on her life than Figure has.
Last edited by George; 17 Apr 2005 at 09:47 PM.
Lordmrw
Rpg Master
Oh hell yes, BAA is the shit! When I started buying manga in 2003, I picked up Last Order Volume 1 on a whim, and I don't ever regret. I started buying the original series to fill the lull between Last Order volumes. The amount of creativity and research that more than likely goes into the series is what has me hooked. I think I've read Last Order volume 5 6 times by now. Interesting that Viz is only releasing 2 volumes a year; I just assumed that LO wasn't done in Japan yet, and that new volumes were released over here as soon as they were done there.
www.classic-games.net updated every Monday, Wednesday, and Friday.
18 Apr 2005, 01:03 AM #7
Ashen Victor
the Crash King
i need to catch up with LO. i've got the first one when that came out, but lack of funds have kept me from getting the rest (and a whole lotta other series, too). i'm also thinking about collecting the rereleases (even though i've already got the original releases), but is there anything in them that make them worth plunking down for (besides the extra info stuff)? and if you want more motorball goodness, then check out Ashen Victor.
great thread Mech.
Five is out now?
Came out on the 12th. Was also the only time I've ever rushed to a bookstore to hope they had something on release day.
The cover of volume 6 has Alita/Gally squatting on top of this big purple mass in outer space, with two arm-blades coming from her forearms a la LO volume 4.
LO6 LO7
Well, he was her only love after the Salem-obsessed kid and he's one of the few interested in Alita's humanity. That's gotta count for something. You also reminded me, I keep wondering when/if Kaos is going to pop back up after his show in LO. I figured there was going to be more with him but they seem to be getting really far away physically so if he does get seen again it probably won't be until the very end.
Also, I need that calender.
Originally Posted by Lordmrw
Interesting that Viz is only releasing 2 volumes a year; I just assumed that LO wasn't done in Japan yet, and that new volumes were released over here as soon as they were done there.
I saw that LO had been getting translated into other languages a year or two before we started getting it (Italian, IIRC) and I thought it had already been wrapped up by now. Seems like I'm wrong since Japan just got LO7 on 03/18/2005 so there could still be more coming.
If only I knew Japanese and could just import them.
Originally Posted by Ashen Victor
but is there anything in them that make them worth plunking down for (besides the extra info stuff)?
Not that I know of. I never owned the originals (I borrowed a friend's collection) so I'll be buying the rereleases at some point, which will line up nicely in size with LO's volumes. It'll also be easy to finally keep track of which volume is which, I could never remember what order they were in by the names alone.
It'll also be easy to finally keep track of which volume is which, I could never remember what order they were in by the names alone.
I hated that. I actually avoided buying the graphic novels when they first came out because of that.
18 Apr 2005, 02:00 AM #10
it actually tells you what volume a particular book is when you open up and read the publishing notes. it was the only way i knew how to buy them, but i didn't start doing that after realizing i skipped the entire motorball arc (going from 1 and 2, to 5 and 6).
oh, and Trial, next time you're in the city and happen to stop by Forbidden Planet, they've got a 3/$24 manga deal happening on their upper level (relegated to anything $10; which should be most of them). noticed it today after hitting up a street fair further up on 17th and Broadway.
Last edited by Ashen Victor; 18 Apr 2005 at 02:04 AM.
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Then we had a fun session wit the Theater of Public Policy. I may have better video to add later in the day. Unfortunately the building was not well wired for broadband so the video is a little choppy – but they are very funny so hopefully the humor translates. It was a good opportunity to laugh at ourselves and the learning that has happened in the last two days.


text:
TI Advocates for Moving Transcoding From the Core
Streaming video and audio formats continue to proliferate, many times with no regard to past formats or future compatibility. As such, transcoding-the act of converting digital video from one file format to another-and transrating-the act of changing bitrates while maintaining the same format or codec-have become a standard part of large-scale streaming media distribution systems. But the ability to transcode or transrate at the point of need, when consumers want to move content from one player or format to another, still continues to lag.
In a new Texas Instruments-sponsored report from IDC, titled Transcoding: The Future of the Video Market Depends on It, the case for transcoding is laid out in detail. While the premise of the report (found here, free registration required)-that the evolution of video entertainment will cease without multi-format transcoding-is a bit overblown, the essence of the report is sound.
Sounding a note from TI's DaVinci playbook, the report synopsis notes that real-time transcoding is the key to growth in the video market:
Multi-format transcoding is the most important challenge to overcome for manufacturers and service providers to solve before realizing the potential tremendous growth in video. Consumers have an insatiable appetite for immersion in entertainment, and transcoding multiple formats in real time will be a necessary function for all future video products to be successful.
TI is well-positioned to take advantage of the growth in video, albeit primarily with on-demand content. As noted in a previous article, TI has moved away from just providing chipsets to providing a solution that allows developers to rapidly implement audio and video solutions. TI's DaVinci platform combined TI's core expertise in digital signal processing (DSP) with software that allowed product developers to monitor the throughput of processes across the DSP.
On top of that, TI also recently added several of its own and key third-party codecs to the DaVinci platform, providing developers with bundled, cost-effective encoding and decoding solutions. Several of TI's chipsets also allow for on-the-fly flashing, meaning that the DSP can play content in one format but then, in a very short period of time, dump the current codec and load another codec. This is especially important for products such as next-generation DVD players (HD DVD or Blu-ray) which are required to allow content playback in MPEG-2, VC-1, or H.264.
TI has not been content to rest on the laurels of DSP flashing, however. The company makes chips that go into everything from cell phones to robust servers, and TI is aware that content encoded and played on its high-end DSPs will choke a low-power chipset in a cell phone, as these small chipsets trade off power for battery life. To solve the problem, TI has begun to evangelize the need for transcoding in order to deliver content to the consumer in a format that is appropriate or desired for a particular playback device.
Jeremiah Golston, CTO of TI's Streaming Media division, has been especially vocal in evangelizing transcoding, sometimes directly and sometimes indirectly. In a recent blog posting on the TI website, Golston paints a scenario in which high definition (1080i) is either too much or too little resolution, opening the door wide for the need for transcoding.
"In some cases, HD is not needed at all," said Golston. "Standard definition is still the best tradeoff in applications like IPTV . . . where limited network bandwidth makes delivering even high-quality SD still a challenge. Conversely, there are cases where HD is not enough. Medical imaging applications such as ultrasound require an even higher resolution than 1080i. State-of-the-art ultrasound applications require 4Kx2K to produce the detail needed to make proper diagnoses."
Golston goes on to say, in a point echoed by the new IDC report, that manufacturers have to consider versatility of design to handle changing consumer demand.
What TI and the new report are espousing, then, is a change in mindset on the part of product manufacturers. Rather than tying a device to one particular format, TI argues that product manufacturers should provide-where appropriate-the ability to play back content in multiple formats on a single device. Barring the ability to do so, TI counters its own argument with a push toward real-time transcoding, either at the core or at the consumer. Either way, TI is positioned to take advantage of both trends.
"Transcoding is a life-or-death issue facing manufacturers and service providers as they try to realize the explosive growth in video entertainment," predicts Gene Frantz, TI's Principal Fellow. "Consumers have an insatiable appetite for immersion in entertainment, and transcoding among multiple formats will be mandatory for all future video products to be successful. Digital signal processing technology will be an essential piece in laying the foundation for transcoding among multiple consumer devices."


Just as important as any auction house strategy is the tools you use. I at one point was completely against using any addon what so ever. In fact all I had installed was Omen and Recount for raiding because it was mandatory (well not recount :P). And you guessed it, I was broke.
So I'm basically going to cheat on todays blog and talk about the addons I personally use.
First up it's the addon we all know and love. Auctioneer Suite is a powerful addon for any auctioneer whether your just an average farmer or trying to manipulate markets and take over your auction house.
One of my personal favorite addons is Auctionator. This addon works similar to Auctioneer but is alot easier on your resources and alot simpler to use. There are 3 main features about this addon that I really like which are the new Buy and Sell tabs and the ability to check all your auctions to see if any are undercut.
To the right is a picture of the sell tab in which I blatently stole from curse so I didnt have to log in and take one myself lol.
You will notice a yellow highlight on the prices. That's where you can select the pricing you want your stuff to undercut and post at. Posting is really similar to auctioneer's posting of breaking up the stacks automatically and posting for you.
The buy feature is extremely convenient for buying things. The same kind of list appears and when you go to buy something off that tab a window pops up asking how much of the item at the price you want to buy. You enter in say 6 for 6 stacks and click buy and viola all 6 stacks are purchased instantly.
The next addon is of course Quick Auctions2. I know every blogger has a blog about QA but its such a powerful tool theres a reason why its mentioned so much. It's only really useful if you carpet bomb glyphs or gems.
The reason I didn't crop this picture was because it's my only picture I had of QA and it just so happens the tool from yesterday's blog was nerd raging on me yet again lol so I figured I'd humor you guys with a good laugh.
I had originally given a brief walkthrough of QA2 until I realized it was nothing compared to what Belsebub, author of The Happy Scribe, had written up. So check out this great guide written by Belse.
That pretty much wraps it up for the AH based addons now to talk about some of the support addons I use.
For your profession window you generally have 2 common addons. ATSW and Skillet. I have both and I use both depending on the situation but I lean towards ATSW as my favorite based on sheer looks. ATSW is pretty much the default tradeskill window modified slightly but is easy to use and really quick to get used to. Skillet on the other hand completely reworks the window into its own window and takes alot longer to get used to. Both are great addons depending on your personal taste and both pretty much do the exact same thing. It just boils down to preferences on the look you want.
The key features to both of these great addons is the ability to create a queue for making your items. You add it into the que and click process and it'll make the things in order. If you queue up say a frostweave bag it will add a bolt of frostweave and a bolt of imbued frostweave before the bag simply by just adding a frostweave bag to the queue.
The second important feature is the ability to automatically purchase reagents from the vendor. Great if your a scribe. Have a bunch of Ink of the Sea on you and head to the ink trader with everything in queue. Click buy reagents at the top of the merchant window and viola it automatically converts your ink of the sea into all the inks needed to make whats in your queue.
Last but not least we have Altoholic. This is another godsend addon especially for those of us who have banker alts to do our dirty work. This addon will tell you who has what on the tooltip of the item. You can even bring up the altoholic window and browse other character's banks and even your banker's guild bank. A definate must have.
Well, I thought today's post was going to be short and sweet but what can I say? There's a ton of great addons out there. And using them definitely gives you an advantage over your competition if their not using them.
Nice post, even though I have most of these addons I find auctionator pretty interesting. What are the main diferences between it and auctioneer?
Yea I figured most of us had the addons but *shrugs* lol.
I will definently take a look at it. Does it work together with auctioneer?
Yes it does :) I was using both for months without any errors.
One little thing in this list is missing... Lil'Sparky's Workshop, which is a must if you are crafting anything from Netherweave Bags to Glyphs to anything relevant.
Ok, maybe not a must, but it's a definite time saver in the planning.


text:
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text:
#ifndef _ASM_X86_AMD_NB_H
#define _ASM_X86_AMD_NB_H

#include <linux/ioport.h>
#include <linux/pci.h>

struct amd_nb_bus_dev_range {
	u8 bus;
	u8 dev_base;
	u8 dev_limit;
};

extern const struct pci_device_id amd_nb_misc_ids[];
extern const struct amd_nb_bus_dev_range amd_nb_bus_dev_ranges[];

extern bool early_is_amd_nb(u32 value);
extern struct resource *amd_get_mmconfig_range(struct resource *res);
extern int amd_cache_northbridges(void);
extern void amd_flush_garts(void);
extern int amd_numa_init(void);
extern int amd_get_subcaches(int);
extern int amd_set_subcaches(int, unsigned long);

struct amd_l3_cache {
	unsigned indices;
	u8	 subcaches[4];
};

struct threshold_block {
	unsigned int		block;
	unsigned int		bank;
	unsigned int		cpu;
	u32			address;
	u16			interrupt_enable;
	bool			interrupt_capable;
	u16			threshold_limit;
	struct kobject		kobj;
	struct list_head	miscj;
};

struct threshold_bank {
	struct kobject		*kobj;
	struct threshold_block	*blocks;

	/* initialized to the number of CPUs on the node sharing this bank */
	atomic_t		cpus;
};

struct amd_northbridge {
	struct pci_dev *misc;
	struct pci_dev *link;
	struct amd_l3_cache l3_cache;
	struct threshold_bank *bank4;
};

struct amd_northbridge_info {
	u16 num;
	u64 flags;
	struct amd_northbridge *nb;
};
extern struct amd_northbridge_info amd_northbridges;

#define AMD_NB_GART			BIT(0)
#define AMD_NB_L3_INDEX_DISABLE		BIT(1)
#define AMD_NB_L3_PARTITIONING		BIT(2)

#ifdef CONFIG_AMD_NB

static inline u16 amd_nb_num(void)
{
	return amd_northbridges.num;
}

static inline bool amd_nb_has_feature(unsigned feature)
{
	return ((amd_northbridges.flags & feature) == feature);
}

static inline struct amd_northbridge *node_to_amd_nb(int node)
{
	return (node < amd_northbridges.num) ? &amd_northbridges.nb[node] : NULL;
}

static inline u16 amd_get_node_id(struct pci_dev *pdev)
{
	struct pci_dev *misc;
	int i;

	for (i = 0; i != amd_nb_num(); i++) {
		misc = node_to_amd_nb(i)->misc;

		if (pci_domain_nr(misc->bus) == pci_domain_nr(pdev->bus) &&
		    PCI_SLOT(misc->devfn) == PCI_SLOT(pdev->devfn))
			return i;
	}

	WARN(1, "Unable to find AMD Northbridge id for %s\n", pci_name(pdev));
	return 0;
}

static inline bool amd_gart_present(void)
{
	/* GART present only on Fam15h, upto model 0fh */
	if (boot_cpu_data.x86 == 0xf || boot_cpu_data.x86 == 0x10 ||
	    (boot_cpu_data.x86 == 0x15 && boot_cpu_data.x86_model < 0x10))
		return true;

	return false;
}

#else

#define amd_nb_num(x)		0
#define amd_nb_has_feature(x)	false
#define node_to_amd_nb(x)	NULL
#define amd_gart_present(x)	false

#endif

#endif /* _ASM_X86_AMD_NB_H */

redpajama_set_name: RedPajamaGithub


text:
Q: Using a variable after if statement Wondering what is faster and/or what is better practice when checking a variable in an if statement and then using it again after the if statement.
Like
if var_A + var_B > 10:
    var_C = var_A + var_B

or
 var_temp = var_A + var_B
 if var_temp > 10:
           var_C = var_temp

sorry for the bad examples, was just wonder which of these is better

A: Certainly the second version is better:

*

*It's faster. The expression is calculated only once.

*It's easier to refactor. You will change the expression only in one place.

*It's more readable. The temporary variable name can tell the meaning of the expression.

A: The third option, my favorite, would be to set it and check for untruthy to set var_C to some fallback
var_C = var_A + var_B
if var_C <= 10:
    var_C = None

no extra variable needed

A: Your second option is the best. Subjectively speaking, it's much easier for the next guy to read and maintain.

redpajama_set_name: RedPajamaStackExchange


text:
Das ATP Challenger Rennes (offizieller Name: Open Blot Rennes, vormals Open de Rennes) ist ein 2006 erstmals ausgetragenes Tennisturnier in Rennes, Frankreich. Nach einer Pause 2016 ist es seit 2017 wieder Teil der ATP Challenger Tour und wird in der Halle auf Hartplatz ausgetragen. Es konnte im Einzel niemand das Turnier mehr als einmal gewinnen. Philipp Marx und Florin Mergea gewannen je zwei Titel im Doppel. Außerdem gelang Philipp Petzschner je ein Sieg im Einzel und Doppel.

Liste der Sieger

Einzel

Doppel

Weblinks

 Offizielle Homepage des Turniers
 Ergebnisarchiv der ATP

Rennes


The Georgia Dome in Atlanta, GA, gets a complete renovation with a new solid foundation by Gepco. The Comprehensive Technical Group performed the installation and system integration.
The Georgia Dome was built in 1992 as a multipurpose stadium and home to the NFL's Atlanta Falcons.When the state-owned facility opened, Georgia Dome Productions was created for all in-house broadcast needs.
Gepco cables provided the foundation for the Georgia Dome's new equipment. The cabling had to be able to handle the analog, digital and HD formats used in the suite.
Any facility associated with the NFL must have broadcasting capabilities that comply with the league's rigorous standards. This meant that the antiquated analog systems in the stadium's control suite had to be upgraded to SDI, and its broadcast infrastructure prepared for an upgrade to high-definition in the future. The suite, operated by Georgia Dome Productions, produces its own in-house show on game day. While it is relied upon heavily for productions, the Georgia Dome has two LED video boards and over 500 monitors, it also receives a broadcast feed from VyVX for league highlights shown on the same monitors. Another aspect of the Georgia Dome that separates it from many other NFL stadiums is its ability to broadcast outside of the facility. The control suite, which can handle uplinks as well as downlinks, has a fiber line that runs directly out of the room to parent company Crawford Communications' satellite teleport.
Most control rooms throughout the NFL are only used from August to January and then are stored away until the next season, but the Georgia Dome is used year-round. It hosts events such as Supercross, NCAA SEC championship football and basketball, NCAA men's and women's basketball, professional bull riding, concerts, and conventions. The facility's full-time use stressed the need for an upgrade to a higher-quality system.
The control room, originally had linear editing equipment supplied by Crawford Communications, including a Grass Valley routing switcher; an 230 Ampex video switcher, an ACE editor and ADO-1000 digital effects from Ampex; an Abekus A42 still store; and BVW75 and BVW65 Beta decks and a ¾-inch VTR from Sony. Since some of the gear was more than 20 years old, it was time to bring the suite up-to-date.
The Georgia Dome chose the Evertz MVP multivideo processor, with three Mitsubishi LCD monitors for display instead of a traditional monitor wall found in most control rooms.
Comprehensive Technical Group (CTG) was contracted by Georgia Dome Productions to perform the installation and system integration. CTG was hired on June 6, 2003 and had to have the room up and running by the Falcons' first preseason game on Aug. 9, 2003. However, the actual installation had to be finished closer to Aug. 1, 2003, to allow the stadium crew a week to become accustomed to the new setup. CTG began with a two-stage design process and turned to an assortment of Thomson Grass Valley products. A Zodiak 64-input production switcher was one of the main units in the installation. Other Thomson Grass Valley units included a Concerto routing switcher, framed at 128x128, but populated at 64x64, and a GVEous DVE. The upgrade also allowed the suite to get away from the traditional monitor wall found in most control rooms and move to an Evertz multiview processor, which is displayed on three Mitsubishi LCD monitors. There are still some standard monitors in the suite for program previews and tests, but the majority of monitoring is handled by the 40-inch LCDs. The Evertz multiview processor is easily reconfigured for the facility's events.
One of the constants when performing the various aspects of the overhaul was the use of Gepco audio and video cables. It's one thing to upgrade to high-tech A/V equipment, but if the material that connects it all is faulty, then the new gear becomes irrelevant. The cabling had to be able to handle the analog, digital and HD formats used in the suite. A combined total of 40,000 feet of Gepco's VPM2000 and VSD2001 cables were used in the upgrade. CTG supplied the suite with four Leitch DPS-575 frame synchronizers in order to integrate feeds into the in-house production. The room also receives feeds from several cameras throughout the stadium, providing the crowd with the same views and angles that the referee has for instant-replay challenges during the game.
ADC video patch panels were chosen for the job since they are rated for HD signals.
With the suite located on the press box level of the stadium, space was at an expensive premium and was a major factor in the room's design. The tight parameters of the room are analogous to what one would find in a large broadcast truck, so it was decided to keep the design and equipment consistent with a standard remote truck. Therefore, this design also provided a familiar layout for the freelancers who are often hired.
In addition to upgrading the production equipment, Georgia Dome Productions also wanted to update the editing equipment. Previously the facility was using an Ampex ACE editor that was physically located in the production control room. An Avid Media Composer was added, and it allows individuals to operate separately from the control room.
To handle the new digital formats, as well as the remaining analog units, the production suite was equipped with a Sony IMX deck, which allows the playback of legacy tape formats such as Beta, Beta SP and DigiBeta. The Sony IMX further increased the facility's versatility and ability to manage multiple formats with ease.
The installer could have brought in enough equipment either to bring the entire control room suite up to date, or to change everything over to HD. Considering the numerous clients that the Georgia Dome services aside from NFL football, CTG opted to upgrade the room, while taking the first step in HD preparation. When the time comes for a complete upgrade to HD, the suite will only need a few extra matrixes for the routing switcher.
As the season closes for the Atlanta Falcons, the upgrade has been a success. The new equipment has been easier to use and created a more reliable production and editing environment. In 2004, the Georgia Dome will play host to the Chick-Fil-A Peach Bowl, Monster Jam and Honda's "Battle of the Bands" 2004 invitational showcase.
Beverly Wilson is operations manager for the Georgia Dome.
Dome Productions has been steadily and progressively adding to its complement of HD production vehicles.
A new PESA router was installed in December 2012 to meet the new demands of Georgia Tech Online's Global Learning Center and to simplify operations.
Calrec Audio's Brio system has found its way under Dome Production's roof as part of a recent studio upgrade.
The University of Georgia Bulldogs of the Southeastern Conference (SEC) has assigned video acquisition for coaching analysis to four Panasonic AG-HPX370 and two AJ-HPX2000 P2 HD shoulder-mount camcorders.