The design and operation of cities is the province of urban planning. But an explosion of startups in cities means a lot of new products and services for urban areas. The problem is, we don't really know how people are going to use these new products and services.
"The company launched a trial service in Santa Monica just last year and when I first saw the scooters (parked literally outside of our office) I was convinced nobody would want to ride them…The volume grew so steadily that I finally hopped on one, rode down to Bird's offices and pleaded with Travis to take money from us. I had literally never seen a consumer phenomenon take off so quickly," says Mark Suster in All The Questions You Wanted Answered about Bird Scooters and Their Recent $300 Million Funding.
Just four-and-a-half years ago, people were stunned by the then huge valuation of Uber at over $3.5 billion. It took Uber just over four years to get to that valuation. Now Uber is acquiring electric, dockless bike companies and investing in shared scooters, as they dial back their self-driving activities. The chart below explains why.
The practice of sharing rides came out of nowhere five years ago, and two years ago, docked bike share seemed to be rewriting what was possible with on-demand transportation. (Let's see if/where scooters show up in Q1:19.) It's hard to appreciate the impact of these new mobility models until you look at them against some well-established existing modes of transportation like taxis and car rentals. These industries trace their roots back to the explosion of the automobile with Model Ts a century ago and to when entrepreneurial companies like Hertz decided taxis should be yellow to enhance their visibility for hailing. (And yes, that's the same yellow Hertz car rental sign.) As the chart below shows, these 100-year-old industries are rapidly melting away in the face of on-demand competition.
What does this mean for city planners? For a long time in the U.S., cars have so dominated public spaces that we've mostly focused on parking and roads. We forget that companies lobbied for the car — they hadn't always dominated public spaces, and now cities around the world are steadily pushing back. With new mobility options come new corporate alliances.
"San Francisco has more than 250,000 on-street parking spaces for 'dockless' cars, so why does the addition of a few thousand dockless scooters spark such a heated debate?" says Roelof Botha, who is also an investor in Bird.
Parking for small shared EVs is just the start. What about the impact of last-mile options on public transit usage? Lyft's "friends with transit" policy could be viewed cynically as a way to win favor with regulators, but last-mile trends are also playing out with smaller on-demand vehicles. In Germany, DB figured out the relationship between bikes and transit more than 10 years ago with the first dockless shared bikes, and the massive bike parking infrastructure connected to Dutch transit.
In the city most associated with car culture, you can now stop by any Metro station along the Expo Line in LA and see a growing number of bikes and scooters. Is this associated with an increase in transit usage? Is this another reason to sort out parking for small, last-mile vehicles? With more venture dollars in the mix, there are now strong alliances seeking to test new approaches.
Just before cars finally took over most public spaces for transportation, there were more public transit options provided by some weirdly familiar looking vehicles. You can almost see how this 1922 Austro Motorette would eventually be given a seat to become the more familiar-looking Vespa.
There are some important differences now. Electric vehicles need new charging infrastructure, which has led to debates about who will pay for it. On the other hand, scooter-sharing companies have learned infrastructure doesn't need to look like charging stations. Small vehicles can have their batteries swapped out (as with the scooter share Coup) or companies can offer incentives to people to take vehicles home to charge (and then return them). Electric vehicles will continue to drop in price as the main cost — batteries — become cheaper. Finally, shared vehicles have never been more available, and electric scooters are almost 100x cheaper than cars. What happens to behavior when availability is so high that it doesn't require you to leave your block to find a vehicle?
It seems inevitable that AVs will replace drivers at some point. While we wait for the takeover, there are some approaches we can take to improve safety. Unfortunately, some of these seem to have unintended negative consequences. Growing up I used to visit Zimbabwe, where speed bumps were called "sleeping policemen" because it was believed that they caused drivers to slow down and obey posted speed limits. But data from a recent NYU and Urban Us portfolio company, Dash, reveal that "drivers have a tendency to accelerate quickly after traffic calming infrastructure like speed bumps, which can lead to dangerous situations for pedestrians." This is potentially a new issue as more drivers discover previously quieter streets via navigation apps and it should still force us to revisit how we try to manage drivers who are going too fast.
With NYC's L train shutting down in 2019, people have started to plan their housing options and new commutes to and from Manhattan. The city has responded by saying they will add additional ferries and CitiBikes. But is there a way to add more options quickly? How might they fare in the winter? It's hard to know, but the consequences go far beyond mobility to impact everything from restaurants to residential real estate.
Mobility ultimately has a lot of consequences for real estate. Are people going to live in smaller private spaces in exchange for better shared amenities? Will they use robotic furniture to get more from smaller spaces? What might cause homeowners to purchase backup power in the form of a home battery system? How will this impact the grid? Will people be OK sharing sidewalks with delivery robots?
With so many questions about how our behavior will change, we need to find better, faster ways to test new solutions. Maybe alongside departments of urban planning, we need departments of urban testing.


text:
Home Tags Grammy award winners
Tag: grammy award winners
World news – Skydiver dead after suspected parachute failure
A 30-year-old man has died after a tragic skydive during a state skydiving competition north of Perth.
World news – Grammys 2021: List of Winners – I Can't Breathe wins song of the year
Grammys 2021: Everything You Need To Know About Music's Biggest Night
World news – See who's up for a Grammy Award tonight
The winners of the 63rd annual Grammy Awards will be announced on Sunday.

redpajama_set_name: RedPajamaCommonCrawl


text:
This Majestic Ghost King Will Burn. And It's Makers Will Be Proud.
by Sharanya Pillai in Alt on August 6, 2016
If there is beauty in creation, perhaps there is just as much in destruction.
With only two helpers, a craftsman spends months building a two-storey effigy, every part painstakingly put together by hand — for the sole purpose of burning it to the ground.
Malaysian air force retiree Ng Chi-Wang runs a Chinese paper offerings business in Bukit Merapit, Penang.
Every year, as part of the Hungry Ghost Festival, he constructs a giant paper effigy of the netherworld guardian Da Shi Ye, otherwise known as the Ghost King.
Ng stays true to his craft in constructing the effigy solely by hand, from using his fingers to glue every piece of paper to sawing every bamboo stick with a hand saw. "Greatest thing is the craftsmanship," he says. "Learning something extra from doing it."
This master craftsman pays close attention to every single detail, undaunted by the sheer scale of the project. When every single piece of paper is pasted on the mold, the resulting figure takes on a life of its own, with ordinary paper turning sacred as the townsfolk kneel before and pay their respects to the formidable Ghost King.
Perhaps inspired by Ng's attention to detail, filmmaker Dick Chua similarly trains his camera on the most intricate of details in his documentary profiling Ng, 'The Ghost King'.
From the close-ups of glowing embers to using high-definition cameras that reveal the texture of bamboo, Chua pays homage to the intricacies of paper art with the technical realisations of his film.
For Ng and his helpers, three months of hard work comes to a conclusion on the fifteenth day of the seventh month, when devotees take Da Shi Ye out on a procession, shower him with paper money. They then pay their final respects, and in reverence, set him alight.
The flames reflected in his eyes, Ng looks on proudly as Da Shi Ye crumbles to the ground, and the ashes float to the heavens.
While he concedes that it is impossible to make a living this way, Ng knows that he will be back with another effigy next year. And the next.
For as long as he can work, the craftsmen is devoted to upholding this larger-than-life tradition.
Watch 'The Ghost King' by Dick Chua (Malaysia) on Viddsee:
Here's another demonstration of faith. Watch this Singaporean drama 'The Kavadi Bearer' on Viddsee
Article by Sharanya Pillai in Alt on August 6, 2016
Tags: chinese culture, Chinese Lunar calendar, D1 Production, dick chua, Ghost King, hell bank notes, hungry ghost month, hungry ghost penang, paper effigies, Penang Bukit Mertajam, tradition, Traditional Crafts, traditional culture, underworld
He's A Zookeeper, Carer. But He Can't Truly Be Free, On The Other Side.
A Cloud Leopard Sculpture Comes Alive All From A Piece Of Paper
It Was More Than The Family Business At Stake. There's Also Heritage, Legacy.
Here's A Woman Travelling Across Israel On A Quest For Knowledge
Meet The Man Who Changed The Lives of 10,000 Rickshaw Pullers in India


Preventing irreversible degradation should be a global fight tackled with local, national and regional solutions. One-third of the world's population lives in drylands where land degradation is reducing food supplies, biodiversity, water quality and soil fertility. Many of the poorest and most food-insecure people live off these lands as small-scale farmers and herders. Because they have no fallback options if this land deteriorates, they are the worst hit by desertification.
Solutions exist to help communities living in harsh environments to improve their livelihoods. The International Crops Research Institute for the Semi-Arid Tropics (Icrisat) is working with local, national and international partners on initiatives that revitalise soils and conserve water, enabling communities to reap the health benefits and incomes from otherwise degraded or soon to become degraded lands.
The approach of bioreclamation of degraded lands shows how women's groups could revitalise barren lands by using simple water and soil conservation techniques, such as zai pits (small holes enriched with compost), to plant drought-tolerant trees and crops, and applying small amounts of fertiliser to the plant root, a technique known as microdosing.
In west Africa, most women have no or few rights to agricultural land, so Icrisat has been working with local NGOs to help them form associations and gain access to communal village wasteland. Scientists showed the women how to plant a range of crops, nutritious trees and high-value vegetables using zai pits and demi lunes (semi-permanent planting basins) to harvest rainwater and concentrate nutrients for the plants.
Their work shows that degraded lands can be made productive by plants such as the hardy Pommes du Sahel, which have 10 times the vitamin C of ordinary apples and are rich in calcium, iron, and phosphorus, and Moringa trees, the leaves of which contain four times the vitamin A in carrots, four times the calcium and double the protein in milk and three times the potassium in bananas. Drought-tolerant pigeon pea was found to help soil fertility by fixing nitrogen in the soil. It also traps pests that would otherwise attack and damage the okra that the women plant in the zai pits, and gives harvests even when rainfall is scarce.
However, most crucially, we must look at how we can prevent soils becoming degraded in the first place. By involving farmers in sustainable water and soil management, Kothapalli, a village in Andhra Pradesh, India, which was previously below the poverty line due to recurrent drought, is now prosperous and serving as a model for other villages in Thailand, Vietnam, China and Africa. Farmers have been shown how to carry out a healthcheck and feed it the nutrients that are missing so that the soil recovers before it is too late. By adding nutrients such as zinc and boron to exhausted soil, farmers are getting better and more nutritious harvests.
Anthony Kapesa has stopped tilling his land. But this farmer from Zombwe village in Malawi still expects a good harvest of maize this year. Faced with worsening dry spells, Mr. Kapesa now spreads moisture-preserving mulch over the surface of his untilled field. Lack of rainfall during the growing season is an increasing concern for farmers in Malawi. Many people believe this problem is due to climate change. In the past, Mr. Kapesa's crops wilted whenever there was a dry spell. He hoed his fields every season. He made ridges on which he planted his maize. But he learned that soil loosened by tilling is more easily dried by the sun. Now, Mr. Kapesa uses wild grass to mulch his fields. He cuts the grass and leaves it to dry before spreading it. To plant his seeds, he pulls aside a little mulch, digs a small hole, drops in a seed, and buries it. Mulch protects the soil against the impact of raindrops. It allows rain to soak slowly into the ground. When the rains don't come, the mulch keeps the soil cool and reduces the rate of moisture loss.
Mr. Kapesa points to a granary full of harvested maize. He says, "Since I started using this system, my crop no longer wilts … as a result, my yields have been more than what they used to be when I planted my crops on ridges." Before he began mulching, Mr. Kapesa harvested 16 50-kilogram bags of maize. Now the same land produces 43 bags, nearly triple the yield.
Tilling the soil and making planting ridges are traditional farming techniques in Malawi. Chakalipa Kanyenda is program manager for Find Your Feet, a UK-based non-governmental organization. Find Your Feet teaches farmers how to adapt to the effects of climate change. According to Mr. Kanyenda, tilling and ridging can increase moisture loss from the soil. He says that mulching has successfully cushioned farmers against the increasingly erratic rainfall in Malawi. Farmers have eagerly adopted the practice.
"They call me 'Mama Poo'" Anne told me matter-of-factly as we strolled through a dusty pathway in Silanga, a small neighbourhood in the expansive Kibera slums of Nairobi, Kenya. "And I like that," she added.
Anne Nudge is a Sales Representative for Peepoople AB, a Swedish social enterprise that, last October, launched a pilot project in Silanga, marketing and selling "The Peepoo"– a single-use, personal toilet that sanitizes human waste quickly, preventing it from contaminating the surrounding environment. After just a few weeks, the bag transforms the waste into a nutrient-rich fertilizer. (This then gets used in bag-gardens – more later). It works because the inner bag contains a cheap chemical urea that breaks down and kills all the bugs in the poor in just 3 weeks. By this time the plactic has biodegraded and you have safe compost.
The second, and less attractive option, are "flying toilets," tiny grocery bags that, after usage, are carelessly thrown into the street or alley, where it seeps back into the ground.


text:
Q: Append element with SAX in python I know how to parse xml with sax in python, but how would I go about inserting elements into the document i'm parsing? Do I have to create a separate file?
Could someone provide a simple example or alter the one I've put below. Thanks.

from xml.sax.handler import ContentHandler
from xml.sax import make_parser
import sys

class aHandler(ContentHandler):

    def startElement(self, name, attrs):
        print "<",name,">"

    def characters(self, content):
        print content

    def endElement(self,name):
        print "</",name,">"

handler = aHandler()
saxparser = make_parser()
saxparser.setContentHandler(handler)

datasource = open("settings.xml","r")
saxparser.parse(datasource)

<?xml version="1.0"?>
<names>
    <name>
      <first>First1</first>
      <second>Second1</second>
    </name>
    <name>
      <first>First2</first>
      <second>Second2</second>
    </name>
    <name>
      <first>First3</first>
      <second>Second3</second>
    </name>
</names>

A: With DOM, you have the entire xml structure in memory.
With SAX, you don't have a DOM available, so you don't have anything to append an element to.
The main reason for using SAX is if the xml structure is really, really huge-- if it would be a serious performance hit to place the DOM in memory. If that isn't the case (as it appears to be from your small sample xml file), I would always use DOM vs. SAX.
If you go the DOM route, (which seems to be the only option to me), look into lxml. It's one of the best python xml libraries around.

redpajama_set_name: RedPajamaStackExchange


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

In the past two decades, thousands of identifiable planets outside
the solar system have already been spotted
\citep[e.g.][]{Vogt00,Pie10,Mou11,Ofir13,Rowe14}. An overwhelming
majority of them have been discovered using indirect methods, i.e.,
radial-velocity (RV) and photometric transits. This is due to the
fact that planets are non-luminous bodies, they merely reflects
light of the parent star. A planet is like a small "undetectable"
speckle in the stellar image, from a distance of a few parsec. But a
planet can cause dynamical perturbations onto parent star, providing
the possibility to detect it by indirect means. As a consequence,
this makes the characteristic parameters of a exoplanet depend
strongly and only on the characteristic parameters of the host star.
Hence, it is of great significance to obtain the accurate masses and
radii of host stars to study exoplanets
\citep[e.g.][]{Sea03,San08,Winn10}.

The most commonly used method for determination of the stellar
properties is to fit the parameters of theoretical models with the
observational constraints, e.g. effective temperature $T_{\rm{eff}}$
and luminosity $L/L_{\sun}$. However, this method generally makes it
difficult to obtain sets of complete stellar atmospheric parameters.
There are a few of free parameters in stellar structure and
evolution models, which bring more uncertainties in the
observations, result in insufficient estimation of the stellar
properties \citep{Bi08}.

Nevertheless, the abundance of lithium in stellar photospheres is
usually used to study various processes, from big bang
nucleosynthesis to the formation and evolution of planetary systems
\citep[e.g.,][]{Mel10,San10}. Lithium is readily destroyed in
stellar interiors at a comparatively low temperature ($\sim$ 2.5
$\times$ 10$^6$ K), therefore in solar-like stars, the surface
lithium abundance was treated as an extremely sensitive diagnostic
for stellar structure and evolution. Additionally, the evolution of
lithium abundance during pre-MS and MS phases have strong
correlations on several properties of star, i.e., metallicity, mass,
age, and rotational history. Meanwhile, due to total angular
momentum loss induced by magnetic braking, the rotational period of
solar-like stars decreases with age during the main sequence. And
the rate of angular momentum loss is related to stellar mass, radii
and rotational rates. Accordingly, by combining non-standard stellar
model which includes the process of extra-mixing with accurate
measurement of lithium abundance and rotational period, we can
obtain more precise estimation about the fundamental parameters of
EH stars and their planets \citep{Do Nascimento09,Cas11,Li12}.

In this work, we computed evolutionary models including
rotation-induced element mixing and microscopic diffusion. We used
three commonly used observation constraints ($T_{\rm{eff}}$,
$L/L_{\sun}$ and [Fe/H]) and two additional observation constraints
(the lithium abundance $\log$ $N$ (Li) and the rotational period
$P_{\rm{rot}}$) as restrictions of stellar models, aiming to provide
the stellar parameters accurately. We assumed that the depletion of
lithium happens at pre-main-sequence (pre-MS) and evolve differently
with different initial rotational rates.

The observed data of the six EH stars and their planets are
summarized in Section ~\ref{sect:Obs}. The computational method and
the details of our evolutionary models are described in Section
~\ref{sect:Mod}. In Section ~\ref{sect:Res}, we present our modeling
results and compare with previous studies. Finally, the discussion

\section{The selection of star sample}
\label{sect:Obs}

\subsection{EH Stars}

\begin{table}
\begin{center}
\caption{Main Characteristics of Six EH Stars.}\label{tbl1}
\begin{tabular}{cccccccc}
  \hline\noalign{\smallskip}
HIP & HD & $T_{\rm{eff}}$ & $\log(L/L_{\sun})$ & [Fe/H] & $\log$ $N$ (Li) & $P_{\rm{rot}}$& ref \\
    &    & (K)            &                    &        & (dex)           &               &     \\
  \hline\noalign{\smallskip}
    9683   & 12661  &  5743$\pm$44 &  0.093$\pm$0.063  &   0.36$\pm$0.03  & ...           & ...        & (1)  \\
           &        &  5785$\pm$50 &  0.033$\pm$0.063  &   0.37$\pm$0.03  & 1.10$\pm$0.60 & ...        & (2)  \\
           &        &  5715$\pm$70 &  ...              &   0.36           & ...           & ...        & (3)  \\
           &        &  ...         &  ...              &   ...            & ...           & 35$\pm$2.1 & (5)  \\
           &        &  5748$\pm$70 &  0.063$\pm$0.063  &   0.36$\pm$0.03  & 1.10$\pm$0.60 & 35$\pm$2.1 & (6)  \\
    \ & & & & & & & \\
    33212  & 50554  &  5929$\pm$44 &  0.167$\pm$0.063  &  -0.07$\pm$0.03  & ...           & ...        & (1)  \\
           &        &  5982$\pm$26 &  0.119$\pm$0.062  &  -0.07$\pm$0.02  & 2.40$\pm$.011 & ...        & (2)  \\
           &        &  6050$\pm$70 &  ...              &   0.02           & 2.59          & ...        & (3)  \\
           &        &  ...         &  ...              &   ...            & ...           & 16$\pm$1.0 & (5)  \\
           &        &  5987$\pm$70 &  0.143$\pm$0.063  &  -0.04$\pm$0.03  & 2.50$\pm$0.11 & 16$\pm$1.0 & (6)  \\
    \ & & & & & & & \\
    47007  & 82943  &  5997$\pm$44 &  0.169$\pm$0.047  &   0.27$\pm$0.03  & ...           & ...        & (1)  \\
           &        &  6011$\pm$36 &  0.152$\pm$0.061  &   0.28$\pm$0.03  & 2.47$\pm$0.10 & ...        & (2)  \\
           &        &  6025$\pm$70 &  ...              &   0.33           & 2.52          & ...        & (3)  \\
           &        &  ...         &  ...              &   ...            & ...           & 20$\pm$1.2 & (5)  \\
           &        &  6011$\pm$70 &  0.161$\pm$0.061  &   0.29$\pm$0.03  & 2.50$\pm$0.10 & 20$\pm$1.2 & (6)  \\
    \ & & & & & & & \\
    50473  & 89307  &  5898$\pm$44 &  0.096$\pm$0.062  &  -0.16$\pm$0.03  & ...           & ...        & (1)  \\
           &        &  5914$\pm$25 &  0.130$\pm$0.063  &  -0.18$\pm$0.02  & 2.18$\pm$0.11 & ...        & (2)  \\
           &        &  ...         &  ...              &   ...            & ...           & 18$\pm$1.1 & (5)  \\
           &        &  5906$\pm$44 &  0.113$\pm$0.063  &  -0.17$\pm$0.03  & 2.18$\pm$0.11 & 18$\pm$1.1 & (6)  \\
    \ & & & & & & & \\
    59610  & 106252 &  5870$\pm$44 &  0.107$\pm$0.069  &  -0.08$\pm$0.03  & ...           & ...        & (1)  \\
           &        &  5923$\pm$38 &  0.108$\pm$0.063  &  -0.05$\pm$0.03  & 1.69$\pm$0.13 & ...        & (2)  \\
           &        &  5890$\pm$70 &  ...              &  -0.01           & 1.65          & ...        & (3)  \\
           &        &  5899$\pm$62 &  ...              & -0.034$\pm$0.041 & 1.71$\pm$0.04 & ...        & (4)  \\
           &        &  ...         &  ...              &   ...            & ...           & 23$\pm$1.4 & (5)  \\
           &        &  5896$\pm$70 &  0.108$\pm$0.069  &  -0.04$\pm$0.04  & 1.68$\pm$0.13 & 23$\pm$1.4 & (6)  \\
    \ & & & & & & & \\
    77740  & 141937 &  5847$\pm$44 &  0.070$\pm$0.073  &   0.13$\pm$0.03  & ...           & ...        & (1)  \\
           &        &  5842$\pm$36 & -0.026$\pm$0.067  &   0.10$\pm$0.03  & 2.26$\pm$0.11 & ...        & (2)  \\
           &        &  5925$\pm$70 & ...               &   0.11           & 2.48          & ...        & (3)  \\
           &        &  5900$\pm$19 & ...               &  0.125$\pm$0.030 & 2.36$\pm$0.02 & ...        & (4)  \\
           &        &  ...         &  ...              &   ...            & ...           & 21$\pm$1.3 & (5)  \\
           &        &  5879$\pm$70 &  0.022$\pm$0.073  &   0.12$\pm$0.03  & 2.37$\pm$0.11 & 21$\pm$1.3 & (6)  \\
  \noalign{\smallskip}\hline
\end{tabular}
\begin{list}{}{}
\item[$^{\mathrm{}}$] Reference: (1) \cite{VF05}; (2) \cite{Ghe10a} and \cite{Ghe10b}; (3)
\cite{Isr04}; (4)\cite{Bau10}; (5)\cite{Wri04}; (6) Mean value.
\end{list}
\end{center}
\end{table}

The sample stars for our modeling are six solar-analog stars with
observed lithium abundances and rotational periods, and their
planets have been detected by using radial-velocity. The detections
of lithium abundances and rotational periods make it is possible to
obtain precise estimations of stellar parameters, especially the
masses and radii which are significant for us to determine the
properties of their planets.

We summarized the observed data of EH stars which were used for our
theoretical calculations in Table ~\ref{tbl1}. The atmospheric
features, $T_{\rm{eff}}$, $L$, and [Fe/H] were collected from
\citet{VF05}, \citet{Ghe10a}, \citet{Isr04} and \citet{Bau10}. We
adopted the lithium abundance $\log$ $N$(Li) from the observations
of \citet{Ghe10b}, \citet{Isr04} and \citet{Bau10}. The rotational
period $P_{\rm{rot}}$ we used was determined by \citet{Wri04} from
the California and Carnegie Planet Search Program with the HIRES
spectrometer at Keck Observatory. The average values of these
observations were adopted in the following study.

The Spectra of \citet{VF05} were obtained with the HIRES
spectrograph mounted on the 10-m telescope at Keck Observatory
\citep{Vogt94}, the UCLES spectrograph mounted on the 4-m
Anglo-Australian Telescope at Siding Spring Observatory
\citep{Die90}, and the Hamilton echelle spectrometer at Lick
Observatory \citep{Vogt87}. The spectra of \citet{Ghe10a,Ghe10b}
were obtained with the FEROS spectrograph mounted on the MPG/ESO
2.20-m telescope at La Silla \citep{Kau99}. The observations of
\citet{Isr04} were carried out using the UES/4.2-m William Hershel,
the SARG/3.5-m TNG at La Palma, and the FEROS/1.52-m ESO, the
CORALIE/1.2-m Euler Swiss at La Silla. Stars from \citet{Bau10} were
observed with RGT spectrograph mounted on the 2.7-m Harlan Smith
telescope at the McDonald observatory, MIKE spectrograph mounted on
the 6.5-m Magellan Clay telescope at Las Campanas observatory, and
HARPS spectrograph mounted on the 3.6-m ESO telescope at La Silla
observatory.

\subsection{Exoplanets}

\begin{table}
\begin{center}
\caption{Main Characteristics of Exoplanets.}\label{tbl5}
\begin{tabular}{lcccc}
  \hline\noalign{\smallskip}
    Planet & $P$ & $e$ & $K_1$ & Ref \\
           &  (day)           &              &   (m s$^{-1}$)     &     \\
  \hline\noalign{\smallskip}
   HD 12661b  &  262.709 $\pm$ 0.083 &  0.3768 $\pm$ 0.0077  &   73.56 $\pm$ 0.56  &   (1)  \\
   HD 12661c  &  1708.0 $\pm$ 14.0   &  0.031 $\pm$ 0.022    &   30.41 $\pm$ 0.62  &   (1)  \\
   HD 50554b  &  1293.0 $\pm$ 37.0   &  0.501 $\pm$ 0.030    &   104 $\pm$ 5       &   (2)  \\
   HD 82943b  &  442.4 $\pm$ 3.1     &  0.203 $\pm$ 0.052    &   39.8 $\pm$ 1.3    &   (3)  \\
   HD 82943c  &  219.3 $\pm$ 0.8     &  0.425 $\pm$ 0.018    &   54.4 $\pm$ 2.0    &   (3)  \\
   HD 82943d  &  1072 $\pm$ 13       &  0 $\pm$ 0            &   5.39 $\pm$ 0.57   &   (4)  \\
   HD 89307b  &  2199 $\pm$ 61       &  0.25 $\pm$ 0.09      &   32.4 $\pm$ 4.5    &   (5)  \\
   HD 106252b &  1600.0 $\pm$ 18.0   &  0.471 $\pm$ 0.028    &   147 $\pm$ 4       &   (2)  \\
   HD 141937b &  653.22 $\pm$ 1.21   &  0.41 $\pm$ 0.01      &   234.5 $\pm$ 6.4   &   (6)  \\
  \noalign{\smallskip}\hline
\end{tabular}
\begin{list}{}{}
\item[$^{\mathrm{}}$] Reference: (1) \cite{Wri09}; (2) \cite{Per03}; (3) \cite{Tan13}; (4) \cite{Bal14}; (5) \cite{Boi12}; (6) \cite{Udr02}.
\end{list}
\end{center}
\end{table}

We listed the planetary orbital parameters which were obtained by RV
measurements in Table~\ref{tbl5}. Two of these systems are found
multi-planetary. HD 12661 and HD 82943 host two and three planets,
respectively. Orbital period $P$, eccentricity $e$, and
semi-amplitude $K_1$ (the velocity wobble) were gave here, for more
details about the planetary such as the periastron passage time $T$
and the angle between the periastron and the line-of-nodes $\omega$
can be found in the related literatures.

The radial velocity data were from the HIRES spectrograph (HD 12661
and HD 82943) mounted on 10-m Keck-1 telescope at the Keck
Observatory \citep{Vogt94}, the ELODIE echelle spectrograph (HD
50554 and HD 106252) and the SOPHIE spectrograph (HD 89307) mounted
on the Cassegrain focus of the 1.93-m telescope at Haute-Provence
Observatory \citep{Bar96}, and the CORALIE echelle spectrograph (HD
141937) mounted on the 1.2-m Euler Swiss telescope at La Silla
Observatory \citep{Que00,Udr00}, respectively.

\section{Stellar Models}
\label{sect:Mod}
\subsection{Input Physics}
To estimate the parameters of the sample stars, a grid calculation
were carried out based on a stellar evolutionary model named Yale
Rotating Stellar Evolution Code (YREC) \citep{Pin90,Pin92,Demarque},
which includes diffusion, angular momentum loss, angular momentum
transport and rotation-induced elements mixing. Detailed
descriptions of model can be found in \cite{Guen92}, \cite{Cha95}
and \cite{Li03}. The calculations were carried out with the
up-to-date OPAL equation-of-state tables EOS2005 \citep{Rogers}.
Solar mixture of GS98 \citep{Grevesse} ($Z_{\sun}$ = 0.0170 and
$(Z/X)_{\sun}$ = 0.0230) was adopted and hence the opacities were
generated with the composition of GS98 \citep{Grevesse} and
supplemented by low-temperature opacities from \citet{Ferguson}.
Atmosphere of the model follows the Eddington $T-\tau$ relation. We
used NACRE reaction rates \citep{Angulo} for nuclear reaction and
the mixing length theory \citep{Bohm} for convection. Following the
formulation of \citet{Thoul}, the gravitational settling of helium
and heavy elements is considered in the stellar model.

When rotation is taken into account, the characteristics of a model
depend on six parameters: mass $M$, age $t$, mixing-length parameter
$\alpha \equiv l/Hp$, two parameters: $X_{\rm{ini}}$ and
$Z_{\rm{ini}}$ described the initial chemical composition of a star,
and rotational period $P_{\rm{rot}}$. To reproduce the evolution of
lithium, evolutions of stars during Pre-MS stage is considered and
hence we selected the initial model for each calculation on the
Hayashi Line. All of the models evolved to exhaust its supply of the
hydrogen in the core. Initial helium abundance ($Y_{\rm{ini}}$ =
0.275) and the mixing-length parameter ($\alpha$ = 1.75) were
regarded as constants in the grid computation.

The ranges of variable parameters of the grid calculation and their
step sizes are shown in Table ~\ref{tbl2}. According to the
effective temperatures of the sample stars, we set the range of mass
from 0.90 to 1.10 $M_{\sun}$ with a grid size of 0.01 $M_{\sun}$.
The range of mass fraction of all heavy elements $Z_{\rm{ini}}$,
which was derived from $Z_{\sun}$ and the observed [Fe/H], is from
0.010-0.040 dex with a grid size of 0.001 dex. Although the initial
models were selected on the Hayashi Line, we used the rotational
rates at zero age main sequence ($V_{\rm{ZAMS}}$) to represent the
rotational conditions for better understanding. The range of
$V_{\rm{ZAMS}}$ is from 20 to 70 km s$^{-1}$, in steps of 10 km
s$^{-1}$.

\begin{table}
\begin{center}
\caption{Input Parameters for Theoretical Calculation.}\label{tbl2}
\begin{tabular}{cccc}
    \hline\noalign{\smallskip}
Variate                            & MIN & MAX & $\delta^{\rm{a}}$ \\
    \hline\noalign{\smallskip}
$M (M_{\sun})$                     & 0.90    & 1.10    & 0.01              \\
Z                                  & 0.010   & 0.040   & 0.001             \\
$V_{\rm{ZAMS}}$ (km $\rm{s}^{-1})$ & 20      & 70      & 10                \\
    \noalign{\smallskip}\hline
\end{tabular}
\end{center}
\tablecomments{0.56\textwidth}{$^{\rm{a}}$ The value of $\delta$
represents the increment between the minimum and maximum values.}
\end{table}

\subsection{Angular Momentum Loss}
The braking law of \citet{Kaw88} is adopted as the angular momentum
loss equation:
\begin{equation}
\frac{{dJ}}{{dt}} = \left\{ \begin{array}{l}
- K{\Omega ^3}{({R}/{{{R_ {\sun} }}})^{1/2}}{({M}/{{{M_ {\sun} }}})^{ - 1/2}}  (\Omega  \le {\Omega _{sat}}) \\
\\
- K\Omega {\Omega _{sat}}^2{({R}/{{{R_ {\sun} }}})^{1/2}}{({M}/{{{M_ {\sun} }}})^{ - 1/2}}   (\Omega  > {\Omega _{sat}}), \\
\end{array} \right.
\end{equation}
where the parameter $K$ is constant for all stars, and associated
with the magnetic field intensity. $\Omega_{\rm{sat}}$ is the
angular velocity of surface when the magnetic saturation occurs in
star. Both $K$ and $\Omega_{\rm{sat}}$ are free parameters and we
follow \citet{Bou97} setting $K$ = 2.0 $\times$ $10^{47}$$\rm{g}$
$\rm{cm^2}$ $\rm{s}$ and $\Omega_{\rm{sat}}$ = 14 $\Omega_{\sun}$.

\subsection{Extra-mixing in the Radiative Region}
Besides the microscopic diffusion of of elements, which we have
mentioned above, angular momentum transport and elements mixing
caused by rotation are taken into account in radiative regions.
These processes can be described as a couple of diffusion equations
\citep{Cha95}:
\begin{equation}
\rho {r^2}\frac{I}{M}\frac{{d\Omega }}{{dt}} = \frac{d}{{dr}}(\rho
{r^2}\frac{I}{M}{D_{rot}}\frac{{d\Omega }}{{dt}}),
\end{equation}
\begin{equation}
\rho {r^2}\frac{{d{X_i}}}{{dt}} = \frac{d}{{dr}}\left[\rho
{r^2}{D_{m,1}}{X_i} + \rho {r^2}({D_{m,2}} +
{f_c}{D_{rot}})\frac{{d{X_i}}}{{dt}}\right],
\end{equation}
where $\Omega$ is the angular velocity, $X_i$ is the mass fraction
of chemical species $i$, and $I/M$ is the moment of inertia per unit
mass. $D_{m,1}$ and $D_{m,2}$ are the microscopic diffusion
coefficients. $D_{rot}$ is the diffusion coefficient caused by
rotation-induced mixing. More details of these diffusion
coefficients were given by \citet{Cha95}. The tunable parameter
$f_c$ was used to alter the effects of rotation-induced element
mixing. It was determined by observations, that is, the depletion of
lithium in our solar model must fits the observed depletion in Sun
\citep{Cha95}.

\section{Results}
\label{sect:Res}

\subsection{Stellar Parameters}

\begin{figure}
\centering
\includegraphics[width=\textwidth, angle=0]{MS1838Fig1.eps}
\caption{Evolutionary tracks of HD 12661, HD 50554, HD 82943, HD
89307, HD 106252, and HD 141937 in the H-R diagram constrained by a)
$T_{\rm{eff}}$ + $L$ + [Fe/H]; b) $T_{\rm{eff}}$ + $L$ + [Fe/H] +
log N(Li); c) $T_{\rm{eff}}$ + $L$ + [Fe/H] + $\log$ N(Li) +
$P_{\rm{rot}}$.} \label{Fig:1}
\end{figure}

we calculated a series of evolutionary models in estimated $M$ and
$Z_{ini}$ ranges to reproduce the observational constraints of these
six EH stars. As shown in Fig. ~\ref{Fig:1}, evolutionary tracks for
each stars are plotted in conformity to observational constraints.
For the sake of simplicity, the situations of star HD 12661 is taken
as an example.

First of all, three classical observed features, the effective
temperature $T_{\rm{eff}}$, luminosity $L$ and metallicity [Fe/H],
were considered and 157 tracks are found fitting these three
observational constraints. The mass and age of HD 12661 provided by
the models are 1.02 $\pm$ 0.03 $M_{\sun}$ and 6.76 $\pm$ 4.31 Gyr.

Secondly, lithium abundance was taken into account. Lithium is the
most important element since it is readily burned in the stellar
interiors. The abundance of lithium indicates the extent of element
mixing in the stars, in addition, the depletion of lithium depends
strongly on the mass and age of star \citep{Do Nascimento09,Li12}.
In this step, there are only 76 evolutionary tracks which fit four
observational constraints, including lithium abundance $\log$ $N$
(Li), and we estimate the mass and age of the star HD 12661 are 1.02
$\pm$ 0.02 $M_{\sun}$ and 5.56 $\pm$ 3.01 Gyr. Additionally, lithium
abundance narrows the ranges of input parameters, thus the possible
position of the star in the H-R diagram is restricted to a smaller
field than what has been obtained above.

Finally, after adding the rotational period to our models as a
constraint, only 30 evolutionary tracks are found fitting the
observed $P_{\rm{rot}}$. The range of $V_{\rm{ZAMS}}$ is
significantly reduced to 30 km s$^{-1}$ - 40 km s$^{-1}$. In a same
way as lithium abundance, the ranges of input parameters of the
stellar models are also reduced by the rotational period, and hence
it makes further constraining to the possible position of the star
in the H-R diagram as shown in Fig.~\ref{Fig:1}a. The rotational
period $P_{\rm{rot}}$ helps us determinate the mass and age of HD
12661 even more precisely, which are 1.02 $\pm$ 0.02 $M_{\sun}$ and
6.39 $\pm$ 1.94 Gyr.

The same method were adopted for all the other EH stars, we plotted
their evolutionary tracks in Fig.~\ref{Fig:1}, each line illustrate
the each star. Comparing the situation of star HD 12661 with others,
we find that this star occupy larger area in H-R diagram than five
other stars in Fig.~\ref{Fig:1}, this is owing to a large error in
the abundance of lithium for HD 12661.

\subsection{Comparison with Previous Results}

\begin{figure}
\centering
\includegraphics[width=\textwidth, angle=0]{MS1838Fig2.eps}
\caption{Comparisons between masses and ages determined by our model
(the black error bar) and estimates of previous studies for all six
EH stars. The red and blue error bars represent the results of
\cite{VF05} and \cite{Ghe10a}, respectively.}\label{Fig:3}
\end{figure}

These six EH stars were previously studied by several researchers,
the methods and estimates of two of them could be seen in
Table~\ref{tbl4}. \citet{Ghe10a} and \citet{VF05} observed these
stars and provided their masses, radii and ages through different
methods. We compare their results obtained by interpolating
isochrones with ours in the following paragraphs. The comparisons of
masses and ages of these six EH stars were plotted in Fig.
~\ref{Fig:3}.

For the six EH stars, the results of \citet{Ghe10a} given the error
of mass is $\sim$ 0.10 M$_{\sun}$ and the error of age is $\sim$ 2.0
Gyr. The mass determinations of \citet{VF05} were close to those of
\citet{Ghe10a} but with higher precision, i.e., $\triangle M$ $\sim$
0.05 M$_{\sun}$. Our mass estimations of HD 12661, HD 50554, HD
82943, HD 89307, HD 106252, and HD 141937 are $1.02 \pm 0.02
M_{\sun}$, $1.04 \pm 0.01 M_{\sun}$, $1.04 \pm 0.01 M_{\sun}$, $1.05
\pm 0.01 M_{\sun}$, $1.03 \pm 0.03 M_{\sun}$, and $1.03 \pm 0.02
M_{\sun}$, respectively, most of which are less massive than what
have been obtained by \citet{Ghe10a} and \citet{VF05}. This result
is due to the element transport which caused by the interaction
between diffusion and rotation-induced mixing in the stellar
radiative region \citep{Cha95,Egg10}. The process of element
transport changes the chemical composition of the external layers
and hence cause the evolutionary tracks shift to hot side on the H-R
diagram. Thus, when the observed effective temperature is given,
rotational model tends to provide less massive result of mass than
those obtained by standard model. The precision of our mass
determinations is the best of the three, which is 0.01 $\sim$ 0.03.

Ages of these six EH stars provided by \citet{VF05} are mostly older
than those of \citet{Ghe10a}, with a similar accuracy, i.e.,
$\triangle t$ $\sim$ 2.0 Gyr. Our age determinations generally agree
within the errors of previous works, and which are much more
accurate ($\triangle t$ $\sim$ 0.5 Gyr) than determined by
interpolating isochrones. (see Table~\ref{tbl4}). Moreover,
Combining the rotational periods listed in Table~\ref{tbl1} with
ages obtained by us, we found that there is a positive correlation
between them.

This result is reasonable, because the depletion of lithium is a
function of stellar mass, age, rotational rates and metallicity,
while the rotational period increases with age during the main
sequence. Therefore, these two additional observational constraints
can effectively restrict the ranges of input parameter and improve
the precision of the stellar model.

\begin{table}
 \centering
  \caption{Stellar Parameters and Comparison with Previous Studies.}\label{tbl4}
\begin{tabular}{cccccc}
\hline\noalign{\smallskip}
Star & $M$          &  t       &  $\emph{R}$  &Method &Ref.\\
     & ($M_{\sun}$) & (Gyr)    & ($R_{\sun}$) &       &    \\
 \hline\noalign{\smallskip}
 HD 12661   &0.96$\pm$0.47            &...                  &1.04$\pm$0.08   & Spectroscopic          & (1)\\
            &1.10$\pm$0.10            &$1.0^{+2.5}_{-1.0}$  &...             & Isochrones             & (1)\\
            &1.22$\pm$0.18            &...                  &1.124$\pm$0.037 & Spectroscopic          & (2)\\
            &$1.13^{+0.05}_{-0.04}$   &$4.2^{+1.4}_{-2.0}$  &...             & Isochrones             & (2)\\
            &1.02$\pm$0.02            &6.39$\pm$1.94        &1.11$\pm$0.08   & This work              &    \\
       &    &    &    &    &    \\
 HD 50554   &0.81$\pm$0.39            &...                  &1.07$\pm$0.08   & Spectroscopic          & (1)\\
            &1.05$\pm$0.10            &$3.5^{+2.5}_{-2.5}$  &...             & Isochrones             & (1)\\
            &0.93$\pm$0.14            &...                  &1.149$\pm$0.039 & Spectroscopic          & (2)\\
            &$1.06^{+0.06}_{-0.05}$   &$4.6^{+2.3}_{-2.5}$  &...             & Isochrones             & (2)\\
            &1.04$\pm$0.01            &2.16$\pm$0.29        &1.02$\pm$0.02   & This work              &    \\
       &    &    &    &    &    \\
 HD 82943   &1.03$\pm$0.50            &...                  &1.10$\pm$0.09   & Spectroscopic          & (1)\\
            &1.20$\pm$0.10            &$1.0^{+1.0}_{-1.0}$  &...             & Isochrones             & (1)\\
            &1.22$\pm$0.17            &...                  &1.125$\pm$0.029 & Spectroscopic          & (2)\\
            &$1.19^{+0.04}_{-0.04}$   &$2.6^{+0.9}_{-1.5}$  &...             & Isochrones             & (2)\\
            &1.04$\pm$0.01            &2.35$\pm$0.33        &1.03$\pm$0.02   & This work              &    \\
       &    &    &    &    &    \\
 HD 89307   &0.85$\pm$0.41            &...                  &1.11$\pm$0.09   & Spectroscopic          & (1)\\
            &1.00$\pm$0.10            &$7.0^{+2.0}_{-2.0}$  &...             & Isochrones             & (1)\\
            &0.91$\pm$0.13            &...                  &1.069$\pm$0.035 & Spectroscopic          & (2)\\
            &$1.01^{+0.04}_{-0.05}$   &$5.4^{+2.6}_{-3.3}$  &...             & Isochrones             & (2)\\
            &1.05$\pm$0.01            &2.31$\pm$0.15        &1.01$\pm$0.01   & This work              &    \\
       &    &    &    &    &    \\
HD 106252   &1.16$\pm$0.57            &...                  &1.08$\pm$0.09   & Spectroscopic          & (1)\\
            &1.05$\pm$0.10            &$3.5^{+2.5}_{-2.5}$  &...             & Isochrones             & (1)\\
            &1.01$\pm$0.15            &...                  &1.093$\pm$0.040 & Spectroscopic          & (2)\\
            &$1.03^{+0.05}_{-0.05}$   &$5.4^{+2.6}_{-3.2}$  &...             & Isochrones             & (2)\\
            &1.03$\pm$0.03            &4.19$\pm$0.65        &1.05$\pm$0.01   & This work              &    \\
       &    &    &    &    &    \\
HD 141937   &0.58$\pm$0.28            &...                  &0.95$\pm$0.08   & Spectroscopic          & (1)\\
            &1.10$\pm$0.10            &$1.0^{+1.0}_{-1.0}$  &...             & Isochrones             & (1)\\
            &1.07$\pm$0.13            &...                  &1.056$\pm$0.039 & Spectroscopic          & (2)\\
            &$1.10^{+0.04}_{-0.04}$   &$4.2^{+1.4}_{-2.2}$  &...             & Isochrones             & (2)\\
            &1.03$\pm$0.02            &2.32$\pm$0.41        &0.99$\pm$0.06   & This work              &    \\
       &    &    &    &    &    \\
 \noalign{\smallskip}\hline
\end{tabular}
\begin{list}{}{}
\item[$^{\mathrm{}}$] Reference: (1) \cite{Ghe10a}; (2) \cite{VF05}.
\end{list}
\end{table}

\subsection{Planetary Parameters}
For a given planetary system with known orbital parameters, we can
calculate the mass function\citep{San08}:
\begin{equation}\label{eq1}
f(m) = \frac{(M_2\sin i)^3}{(M_1+M_2)^2} = 1.036 \times
10^{-7}K_1^3(1-e^2)^{(3/2)}P
\end{equation}
where $M_1$ and $M_2$ are the masses of the star and planet, $i$ is
the inclination of the line of sight with respect to the orbital
axis, $K_1$ is the semi-amplitude of radial-velocity of the star
with mass $M_1$, $e$ is the orbital eccentricity, and $P$ is orbital
period.

Furthermore, as we know, from Kepler's third law:
\begin{equation}\label{eq2}
\frac{a^3}{P^2} = \frac{G(M_1+M_2)}{4\pi^2}
\end{equation}
where \textit{a} is orbital semimajor axis and \textit{G} is the
universal gravitational constant.

From Equation~\ref{eq1} and ~\ref{eq2}, and combined stellar masses
determined in the previous section, the minimum masses $M_2\sin i$
and orbital semimajor axes $a$ of planets can be obtained, as shown
in Table~\ref{tbl6}. It should be noted that the uncertainty of our
estimation consists of two parts. One is associated with the
observation, such as the errors of $P$, $e$, and $K_1$ (listed in
Table~\ref{tbl5}). The other is produced by the model, specifically,
the error of stellar mass. We summarized the two parts of the
uncertainty separately in Table~\ref{tbl6}. Compared with the
results of previous studies, our determinations are more accurate,
whether including the errors of observations or not.

\cite{Bat13} pointed out that a 0.1 $M_{\sun}$ companion would
induce a systematic error of approximately 2\%. Correspondingly, the
accuracy and precision of parameters of EH star will have a huge
impact on our estimates of properties of planet. Therefore, the
accurate knowledge of EH star is extremely important for the study
of exoplanets.

\begin{table}
\begin{center}
\caption{Planetary Parameters and Comparison with Previous
Studies.}\label{tbl6}
\begin{tabular}{l|ccc|cccccc}
  \hline\noalign{\smallskip}
           & \multicolumn{3}{c|}{Previous Studies} & \multicolumn{6}{c}{This Work}\\
    Planet &  $M\sin i$  & $a$ & Ref &  $M\sin i$   & $\delta_M^{obs}$ & $\delta_M^{theo}$ & $a$ & $\delta_a^{obs}$ & $\delta_a^{theo}$\\
           & $(M_{\rm{Jup}})$ & (AU)&     & $(M_{\rm{Jup}})$ & $(M_{\rm{Jup}})$ & $(M_{\rm{Jup}})$ & (AU) & (AU) & (AU)  \\
  \hline\noalign{\smallskip}
   HD 12661b  &  2.30 $\pm$ 0.19   &  0.831 $\pm$ 0.048       & (1) & 2.176 & 0.024 & 0.028 & 0.8079 & 0.0001 & 0.0052 \\
   HD 12661c  &  1.92 $\pm$ 0.16   &  2.90  $\pm$ 0.17        & (1) & 1.812 & 0.042 & 0.023 & 2.8145 & 0.0153 & 0.0182 \\
   HD 50554b  &  5.16              &  2.41                    & (2) & 4.954 & 0.388 & 0.031 & 2.3530 & 0.0446 & 0.0075 \\
   HD 82943b  &  1.59              &  1.1866                  & (3) & 1.500 & 0.067 & 0.009 & 1.1510 & 0.0053 & 0.0036 \\
   HD 82943c  &  1.58              &  0.7423                  & (3) & 1.500 & 0.071 & 0.009 & 0.7209 & 0.0017 & 0.0023 \\
   HD 82943d  &  0.294 $\pm$ 0.031 &  2.137 $\pm$ 0.017       & (4) & 0.278 & 0.030 & 0.001 & 2.0766 & 0.0167 & 0.0066 \\
   HD 89307b  &  2.0 $\pm$ 0.4     &  3.34 $\pm$ 0.17         & (5) & 2.074 & 0.356 & 0.013 & 3.3632 & 0.0619 & 0.0106 \\
   HD 106252b &  7.56              &  2.70                    & (2) & 7.613 & 0.364 & 0.147 & 2.7033 & 0.0202 & 0.0259 \\
   HD 141937b &  9.7               &  1.52                    & (6) & 9.316 & 0.306 & 0.120 & 1.4877 & 0.0018 & 0.0095 \\
  \noalign{\smallskip}\hline
\end{tabular}
\begin{list}{}{}
\item[$^{\mathrm{}}$] Reference: (1) \cite{Wri09}; (2) \cite{Per03}; (3) \cite{Tan13}; (4) \cite{Bal14}; (5) \cite{Boi12}; (6) \cite{Udr02}.
\end{list}
\end{center}
\end{table}

\section{Discussion and Conclusion}
\label{sect:Con}

We made an investigation of the physical state of the six EH stars
and their own planet, by employing the method presented by \citet{Do
Nascimento09}. In the context of commonly observations we added two
observational constraints, the lithium abundance $\log$ $N$ (Li) and
the rotational period $P_{\rm{rot}}$, as constraints to better
determine the fundamental parameters of EH stars and their planets.

We gave the estimations of stellar masses and ages using only the
effective temperature $T_{\rm{eff}}$ and luminosity $L/L_{\sun}$ as
observation constraints. The uncertainties of the mass and age are
approximately 0.05 $M_{\sun}$ and 4.0 Gyr. As we considered the
lithium abundance $\log$ $N$ (Li) and rotational period
$P_{\rm{rot}}$ in our analysis, we obtained more precise
determinations. The lithium abundance helped us to minimize the
errors of masses and ages to 0.03 $M_{\sun}$ and 3.0 Gyr,
respectively. Additionally, we used the rotational period
$P_{\rm{rot}}$ to restrict stellar models based on the former
results. The precision has been improved with $\Delta$M $\sim$ 0.02
$M_{\sun}$ and $\Delta$t $\sim$ 0.5 Gyr. Furthermore, because of the
precise determination of age, we restricted atmospheric
characteristics more strictly than the observations, and positioned
the stars more exactly in the H-R diagram. Furthermore, we obtained
the accurate planetary parameters, i.e., minimum masses $M_2\sin i$
and orbital semimajor axes $a$ by using RV measurements and stellar
masses determined previously.

If we want to completely characterize a system, and obtain accurate
properties of the planet, i.e., the mass, radius, and density, we
need the photometric transit, the RV observations and the properties
of EH star. In the future, we hope to conduct further studies with
the data from Gaia mission.

\begin{acknowledgements}
This work is supported by the grants 10933002, 11273007 and 11273012
from the National Natural Science Foundation of China, and the
Fundamental Research Funds for the Central Universities.
\end{acknowledgements}

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text:
Andreas Wolf (Cyrillic: Андрей Андреевич Вольф, romanized: Andrey Andreyevich Volf; born 12 June 1982) is a German former professional footballer who played as a defender. He spent nine seasons at 1. FC Nürnberg captaining the team for many years before leaving for Werder Bremen in the summer of 2011. In January 2012, he moved to AS Monaco where he played until summer 2014.

Following an end to his playing career, Wolf has since moved to coaching.

Career

1. FC Nürnberg
After moving to Germany with his parents in 1990 Wolf started playing football for several teams in the Ansbach area before joining 1. FC Nürnberg in 1997. There he played for several junior teams, before breaking into first team football in 2002 when he debuted in the Bundesliga against Hertha on 23 March 2002, which saw Nürnberg lose 2–0. He went on to make three more appearances later in the 2001–02 season while Nürnberg finished in 15th place. Despite initially wanting to leave the club, Wolf eventually stayed at the club by signing his first professional contract, keeping him until 2004.

In the 2002–03 season, Wolf spent the start of the season away from the first team and played for the reserve side instead, also being sidelined due to an ankle injury. On 7 December 2002 he made his first appearance of the season, setting up one of the goals in a 2–2 draw against Energie Cottbus. Despite suffering another injury later in the season, Wolf returned to the first team, but was unable to help the club survive relegation in the 2002–03 season during which played in 18 games for the "Club".

In the 2003–04 season, Wolf became a first team regular during Nürnberg's successful promotion campaign, playing in 31 of 34 games. At the start of the season, he was involved in the first team for the first six matches until his sending off for a second bookable offence, in a 1–1 draw against Greuther Fürth on 22 September 2003. He remained in the first team with his performances earning him a new contract until 2006. He scored his first Nürnberg goal on 2 April 2004, in a 2–1 loss against Jahn Regensburg.

In the 2004–05 season, Wolf remained in the first team at the start of the season until he suffered a muscle injury that kept him out for two months. After making his return from injury in a 3–1 loss against Bochum on 27 November 2004, he was sent off for a second bookable offence in the next game on 3 December 2004, a 2–2 draw against Bayern Munich. As the 2004–05 season progressed, Wolf suffered a shoulder injury that kept him out for the rest of the season. He finished the 2004–05 season making 18 appearances in all competitions.

In the 2005–06 season, Wolf recovered from injury and found himself competing over a centre–back position with Thomas Paulus and Bartosz Bosacki. After featuring in three matches since his return in September, he suffered an injury that kept him out for a month. Following his recovery from injury, he returned to the first team, but was plagued with another injury. Wolf again returned to the first team and finished the season making 22 appearances in all competitions. During the season, he signed a contract extension with the club, keeping him until 2009.

With the start of the 2006–07 season, Wolf was back in the starting line-up alongside fellow centre-back Gláuber. He started the season well and helped the club go undefeated in the first nine matches of the season before losing 2–1 against Hertha BC on 4 November 2006, in which he was suspended after picking five yellow cards this season. Wolf's performance continued to impress, resulting him to sign a contract extension keeping him until 2011. He then scored his first goal of the season on 28 April 2007, in a 1–1 draw against Wolfsburg. Although he missed out again due to a back injury he finished the 2006–07 season making 35 appearances in all competitions.

In the 2007–08 season, Wolf continued to be in the first team at the club and scored his first goal of the season on 1 September 2007, in a 1–1 draw against Energie Cottbus. His second goal came on 11 November 2007, in a 3–1 loss against Arminia Bielefeld. Nine days later, on 20 September 2007, Wolf made his European debut for the club, playing the whole game in a 0–0 draw against Rapid București in the first leg of UEFA Cup first round. He suffered injury setbacks in the first half of the season, and later in the 2007–08 season he was suspended twice. The season saw Nürnberg relegated back to 2. Bundesliga with Wolf making 30 appearances and scoring twice in all competitions.

In the 2008–09 season, Wolf stayed at the club amid speculations linking him to a transfer to La Liga side Racing Santander. Following this, he was appointed the new captain. In the opening game of the season, he scored his first goal of the season, but was substituted off having ruptured his anterior cruciate ligament in the 70th minute. After the match, it was announced that Wolf would be out for six months. He made his return to training in February and returned to the first team on 22 February 2009, starting and playing 74 minutes in a 1–0 win over Wehen Wiesbaden. He was given a handful of first appearances until he suffered a knee injury and was substituted as a result in the second half of a 2–0 win against Koblenz on 3 April 2009. Following the match, it was announced that Wolf would be out for the rest of the season after undergoing an operation on his knee. He finished the 2008–09 season making eight appearances in all competitions. During his absence, the club was able to reach the Bundesliga for the next season.

In the 2009–10 season, Wolf returned to the first team from injury in the pre–season and retained his captaincy ahead of the new season. He was featured in the first team for the side at the start until he was suspended for two matches after being involved in an incident in a friendly match. His return from suspension against Bochum on 25 September 2009 was short–lived when he suffered an injury during the match. After spending weeks on the sidelines, Wolf returned to the first team on 17 October 2009, in a 3–0 win over Hertha BC. As the 2009–10 season progressed, Wolf remained in the first team for the rest of the season despite being absent twice and finished the season making 32 appearances in all competitions.

In the 2010–11 season, Wolf remained the club's captain this season and started the first five matches of the season until his sending off after a second bookable offence in a 2–1 win over Stuttgart on 22 September 2010. After serving a one match suspension, he scored two goals in two matches against Schalke 04 and St. Pauli. He scored his third goal of the season in a 3 –1 win over Hannover 96 on 18 December 2010. Wolf continued to be in the first team as the 2010–11 season progressed while being suspended twice and finished the season making 34 appearances and scoring three times in all competitions.

During the 2010–11 season, Wolf's future at Nürnberg was in doubt after the contract negotiation between the two parties had stalled and by mid-May 2011 this had not changed.

At the end of May, Wolf announced that no agreement had been found.

Werder Bremen
On 3 July 2011, Wolf moved to Werder Bremen on a two-year contract, ending his fourteen years association with Nürnberg.

He made his Werder Bremen debut in the opening game of the season, starting and playing the full 90 minutes in a 2–0 win over Kaiserslautern. He suffered an injury in the next match, but was able to return to the next game against Freiburg on 20 August 2011. On 17 September 2011, he played in a 1–1 draw against his former club Nürnberg. In a 1–1 draw against Augsburg on 21 October 2011 he set up Claudio Pizarro to score the equaliser.

By January, Wolf made 15 appearances and announced his desire to leave the club citing injury concerns and personal reasons as the main factors. He had previously stated that he intended to finish his career at Werder Bremen.

Monaco
On 23 January 2012, Wolf signed a two-year contract with an option of extending for a further year with AS Monaco in the French Ligue 2 for an undisclosed fee.

After recovering from an injury sustained whilst at Werder Bremen he made his Monaco debut on 23 March 2012, starting and playing the full 90 minutes in a 2–1 win over Châteauroux. This was followed up against Le Mans on 30 March 2012. However, Wolf suffered an injury again when his face was fractured during the match sidelining him for the rest of the season.

After making two appearances for the club in the first half of the 2012–13 season, it was announced that Wolf was appointed new captain of Monaco, under the new manager Claudio Ranieri. His first game as captain came in the opening game of the season, where he started and played the whole match, in a 4–0 win over Tours. He scored his first goal for the club on 30 September 2012, in a 2–2 draw against Gazélec Ajaccio and his second goal for the club came on 10 November 2012, in a 2–2 draw against Auxerre. Despite being appointed captain, Wolf's first team playing time soon became limited due to new signings as well as his own injuries. While on the sidelines, he said he was treated as a "poor man" at the club. In his second season he made 32 appearances and scoring twice in all competitions.

In the 2013–14 season, Wolf had his captaincy replaced when the club signed Eric Abidal ahead of the new season. After no involvement in the first team in the first half of the season, he was on the verge of joining Dutch side Utrecht In January 2014, but the move was not completed and he stayed at the club for the rest of the season. He appeared as an unused substitute on 10 May 2014, in a 2–1 win over Valenciennes and made his first and last appearance of the season in the next match, the last of the season, coming on as a substitute in the second half of a 1–1 draw against Bordeaux.

After two years at Monaco, Wolf was released by the club.

Post-football career
After leaving Monaco, Wolf retired from professional football and intended to take up coaching instead. Two month later, he returned to Germany, joining his former club Nürnberg as a coach to the junior team. In May 2016, he left the club when he and Roger Prinzen were replaced by Michael Köllner.

Personal life
Born in Leninabad, Soviet Union, Wolf moved to Germany, along with his father, mother and sister. In June 2008, Wolf married his girlfriend Sandra. Together, the couple had a daughter, who was born in 2009.

In 2010, the supporters of 1. FC Nürnberg voted Wolf second behind Stefan Reuter as the club's greatest defenders of the century on the club's website.

Career statistics

Club

Honours
Monaco
 Ligue 2: 2012–13

1. FC Nürnberg
 2. Bundesliga: 2003–04
 DFB-Pokal: 2006–07

References

External links

1982 births
Living people
People from Khujand
Association football defenders
German footballers
1. FC Nürnberg players
SV Werder Bremen players
AS Monaco FC players
Bundesliga players
2. Bundesliga players
Ligue 1 players
Ligue 2 players
Russian and Soviet-German people
Tajikistani people of German descent
Citizens of Germany through descent
Soviet emigrants to Germany
Tajikistani emigrants to Germany
German expatriate footballers
German expatriate sportspeople in Monaco
Expatriate footballers in Monaco

redpajama_set_name: RedPajamaWikipedia


text:
Irish History Made In Plovdiv On Super Saturday
Saturday's proceedings at the greeny-brown lake by the Maritsa River started with a para-glider buzzing the course, continued with some surreal IOC presence in the Paddington-like form of President Bach, and came to a head with several epic A-finals in both the Paralympic and Olympic classes. The Irish made history, the Italians made further leaps up the medal table, Belgium won a rare bronze and while some had their hopes dashed, others fulfilled their destiny with ecstatic gold.
Photo Paul O'Donovan relaxes on the medal pontoons after winning historic gold in Plovdiv.
Fiercely competitive B-finals started the morning, and were rounded off by the novel sight of the current Olympic gold, world gold and world silver medallists in the M4x race for places 7-12. It doesn't take a mindreader to see that those countries who made the quads A-final will have serious targets on their backs in 2019. But in a sport where close and intense competition has become the norm in every Olympic boat category (and quite a few of the others), who won't. Even in the women's quads A-final, where the top four took an early lead they kept extending without positions changing, there was a tension to the race as Poland, who eventually took the gold over Germany and the Netherlands with China underperforming, chipped steadily away to pull out without every quite managing to drop their rivals.
Keep up with all Row360 world championship coverage this week here.
Earlier in the morning IOC President Thomas Bach, visiting Bulgaria as it conveniently hosted three separate sport world championships in one weekend (the others were volleyball and gymnastics), had met athletes, officials and national federation representatives for discussions about the future. He was carefully ushered to watch the A-finals, including two brilliant lightweight doubles races, and was diplomatic about how good everything was in a press conference later on.
Photo Romanians Ionela-Livia Cozmiuc and Gianna-Elena Beleaga – two of only six competitors in Olympic crews who managed to successfully defend a 2017 title.
The lightweights played their part in this PR exercise by delivering beautifully close competitions in both finals. Roumanians Ionela-Livia Cozmiuc and Gianna-Elena Beleaga were two of only six competitors in Olympic crews who managed to successfully defend a 2017 title, surfing the tide of a blistering lightweight doubles final to come out on top, just. The first leaders were Britain, valiantly pushing out in an unanswerably necessary strategy to try and get an edge, but even though Roumania turned the screw and moved through relatively early on, nobody was being dropped rapidly. Just as the Netherlands seemed to be finding a route past the Swiss and Brits, up came the US on a sensational charge which took them through to silver in a near-photofinish with the Dutch. Britain faded but so even more did 2017 runners-up New Zealand.After the Wednesday LM2x kerfuffle it was quite a relief to reach the medal race without any further problems.
"After the Wednesday LM2x kerfuffle it was quite a relief to reach the medal race without any further problems."
Rachel Quarrell
After the Wednesday LM2x kerfuffle it was quite a relief to reach the medal race without any further problems. Unfortunately before racing began Norway's Kristoffer Brun had to drop out for medical reasons and so Are Strandli moved to bow and Jens Holm was brought in to stroke. They kept up with the race for the first half but couldn't hold the speed and dropped back with Spain while the rest forged on. Italy kicked off the fireworks at the front with a great first thousand, but the onlookers were just waiting to see when Ireland's O'Donovan brothers, stalking along behind, would drop the hammer. The answer was just after halfway, and a sense of inexorable power flowed out of the famous siblings, moving them past Italy as if on an express train. But Stefano Oppo and Pietro Ruta stubbornly refused to give up, making the last few hundred metres fast, furious and never quite appearing predictable until the line finally arrived. A history-making first ever Olympic-class world title for Ireland put them on the front pages of every Irish newspaper the next day, albeit with both the French and Norwegians missing from the party, but a major victory for the O'Donovans nevertheless.
Photo Corne de Koning and Annike Van der Meer teamed up to bag the PR2 mixed double gold.
Not content with PR2 singles gold and silver respectively, Corne de Koning and Annike Van der Meer teamed up to bag the PR2 mixed double gold as well, in a race which looked widely spread by the end but was surprisingly competitive early on. They were a second off a world best time in an average tail-wind — and don't forget this is not a new boat class but a seasoned Paralympic event — and could almost certainly have broken it if pushed harder. But minutes later we were treated to an insanely competitive mixed coxed fours final, in which Britain won their eighth successive gold to consolidate the longest active winning streak, after being pushed almost to breaking point by the USA.
The American para-four, including indomitable stroke Danielle Hansen who later rowed another whole flat-out final to claim an automatic gold at bow in the uncontested PR3 women's pair, dashed off the blocks at high speed, clearly hoping to put the Brits under pressure. For a while they kept the upper hand, while Britain concentrated on settling into their best rhythm. With that as a springboard, the defending champions began their pushes before half-way, and then simply kept pushing, capping everything the US could try until they finally got their bows over the line. It was hard, it was brutal, there were never more than a few feet in it and because of the doubled distance, it was by far the toughest mixed coxed fours race since the boat class was invented. And given that both the GBR and USA fours intend to stay in the game until Tokyo, it could get even more interesting next year.
Photo The women's pairs saw relative newcomers Caileigh Filmer and Hillary Janssens from Canada beat the New Zealand headline duo.
New Zealand have shown signs of slipping off their high standards this year, with both eights in the B-finals and Kiwis losing close semi-finals. The women's pairs saw relative newcomers Caileigh Filmer and Hillary Janssens from Canada beat the New Zealand headline duo of Grace Prendergast and Kerri Gowler for the second time this week, having given them fair warning with a blistering semi-final defeat. Nobody else got a look-in as these two barrelled towards the line lengths and lengths clear, and the message was clear: the new girls are in town.
Photo Croatia's Sinkovic brothers.
By contrast the men's pairs, which could have been close, were a one-boat party for Croatia's Sinkovic brothers, pulling out what may very well be their best ever race in the pair. Once the field had sorted itself out behind them, Roumanians Cozmiuc & Tudosa and the Onfroy brothers from France threw the kitchen sink at trying to overturn the Croatian lead, but despite impressively fast final sprints this time they couldn't find a single chink in the Sinkovic armour.
Photo US registering a deserved close victory over defending champions Australia while Russia
Sweep continued to produce epics: the women's four ended in a hell-for-leather sprint and the US registering a deserved close victory over defending champions Australia while Russia picked up bronze. The W4- has come on a very long way since the start of its inclusion in the Olympic classes in May 2017, and fully deserves its place at the top table: the US led all the way and matched anything the Aussies could throw at them. Green and gold order was restored a race later, as the Australian men's coxless four did manage to retain their title, at first looking as if they would do it with lordly grandeur a length ahead of the rest. Going past 1600m a switch flicked in the brains of the Italian M4- in the adjoining lane, and suddenly a brilliantly bonkers Italian sprint was in full swing, rapidly chewing up the water between them and the Aussies. The defending champions held on but only just: 0.25 seconds is nothing at this level and they were fading very fast in the last 50 metres, grimly waiting for the line. The British four, who had already won their battle against the Netherlands for bronze, also closed quickly on the leaders, while Roumania's under-23 champions were left struggling in fifth ahead of Germany. One Australian athlete had to skip the medal ceremony, exhausted, a measure of how much had been expended to seal the win.
Photo Italian men's quad win gold in the last race of Saturday's A-finals
Italy's party went up another gear in the last race of the A-finals, when they pulled a blinder to grab the men's quads gold from lane 1, catching everyone else unawares and hoicking them back to the top of the medal table. The sight of all six quads within a length of each other for most of the course was impressive, and although Australia had a thundering second thousand which helped them clinch the silver over Ukraine, it couldn't quite dent the unshakeable Italian confidence. The bounciness continued into the medal ceremony, with the Italians singing their national anthem loudly and the bow-man conducting the crowd to join in.
Plovdiv World Championships 2018


Requested from DENR by Mary Joy Bultron at 01:55 PM on Mar 30, 2019.
Good afternoon po, need ko lang po sana malaman if may document  po sa department niyo ang pag classify ng indoor air quality and statistics po or may batas at standards po ba ang Pilipinas about dito.
Thank you for your request dated Mar 30, 2019 under Executive Order No. 2 (s. 2016) on Freedom of Information in the Executive Branch.
You asked for Indoor Air Quality Standard.


Our 2015 Far Niente Chardonnay presents fresh and bright aromatics of tropical fruit, melon and hints of fig. This vintage is beautifully balanced by lightly toasted oak. A silky entry develops into a smooth and rich midpalate. Deep flavors of toasted nuts support the bursting flavor of melon and light citrus accompanied by a long and mouth-filling finish.


Dubai - March 20, 2019: Zoho, a global provider of cloud-based business software, today announced its plans for expanding and reinforcing its presence in the UAE and GCC region. The announcement was made on the sidelines of the company's annual user conference, Zoholics Dubai. The initiatives include launch of Zoho's Arabic website zoho.com/ar, and alliance with PayTabs, a Bahrain-based company that will help businesses with payment processing.
Businesses will be able to accept online payments from its customers effortlessly.
Customer payments and transaction fees are captured separately in a clearing account in Zoho Books improving record keeping and the reconciliation process.
With multi-currency support businesses can accept payments in 168 currencies.
Businesses can provide multiple payment methods to their customers. In addition to the traditional options like Visa and MasterCard, businesses can offer regional payment methods like SADAD and MADA in KSA, OmanNet in Oman, and KNet in Kuwait.
'The aim is to help startups focus on building a profitable business from the ground up using industry standard and world-class tools while putting their hard-earned money into their products," said Ali Shabdar, Business Development Director MEA, Zoho Corp. "Startups can stay for at least a year on the platform with no strings attached. However, we expect that within a year or so, a successful startup to come out of the early stages showing signs of revenue backed by our powerful system in the back-end to help them grow faster. At that stage we would ask them to consider paying for the service and support them with their specific needs,' he added.


As a student in Newcastle during the early 1980's Tim developed his love for photography. After having a number of second (or more) hand cameras his first proper one was a Yashica FR1. This along with numerous inspirational visits to the Side Gallery, led to a large collection of black and white images, all self developed.
From there largely due to cost Tim experimented with colour slides, and soon a large collection of these developed. The strong form of the urban landscape, contrasting with the regeneration that was going on at the time in the North East was a strong influence.
Moving to the present day, rather than focusing on how man has tamed his environment, Tim focuses on how nature is interacting with that environment, be it human or natural. This has lead to his "wild-scape" style of photography, which is largely as a result of the "in your face" wild nature that can be found around where he is living.


text:
// INScrollView.h
//
// Copyright (c) 2014 Sven Korset
//
// Permission is hereby granted, free of charge, to any person obtaining a copy
// of this software and associated documentation files (the "Software"), to deal
// in the Software without restriction, including without limitation the rights
// to use, copy, modify, merge, publish, distribute, sublicense, and/or sell
// copies of the Software, and to permit persons to whom the Software is
// furnished to do so, subject to the following conditions:
//
// The above copyright notice and this permission notice shall be included in
// all copies or substantial portions of the Software.
//
// THE SOFTWARE IS PROVIDED "AS IS", WITHOUT WARRANTY OF ANY KIND, EXPRESS OR
// IMPLIED, INCLUDING BUT NOT LIMITED TO THE WARRANTIES OF MERCHANTABILITY,
// FITNESS FOR A PARTICULAR PURPOSE AND NONINFRINGEMENT. IN NO EVENT SHALL THE
// AUTHORS OR COPYRIGHT HOLDERS BE LIABLE FOR ANY CLAIM, DAMAGES OR OTHER
// LIABILITY, WHETHER IN AN ACTION OF CONTRACT, TORT OR OTHERWISE, ARISING FROM,
// OUT OF OR IN CONNECTION WITH THE SOFTWARE OR THE USE OR OTHER DEALINGS IN
// THE SOFTWARE.

/**
 A UIScrollView subclass which adds the feature to cancel touches on certain view objects or on views of specific class names when dragging.

 This class overrides touchesShouldCancelInContentView: and uses the properties classesToCancelTouchesOn and viewsToCancelTouchesOn to determine if a touch should be cancelled when dragging.
 */
@interface INScrollView : UIScrollView

/**
 Array with NSString objects of the class names to cancel touches on when dragging.

 Normally a scroll view will not cancel touches on buttons, though by adding the class name of UIButton to this list will do this.
 The method touchesShouldCancelInContentView: will return true if the touch is on a class which is listed in this array.

 Example of creating the array:

    scrollView.classesToCancelTouchesOn = @[NSStringFromClass([UIButton class])];

 This list may be used in conjunction with viewsToCancelTouchesOn and offers the possibility to cancel all types of objects at once.
 The string will be compared with the string of the view's class name, so there won't be an exception if the given class name doesn't exist.

 @see viewsToCancelTouchesOn
 */
@property (nonatomic, strong) NSArray *classesToCancelTouchesOn;

/**
 Array with UIView objects which to cancel touches on when dragging.

 Normally a scroll view will not cancel touches on buttons, though by adding the object to this list will do this.
 The method touchesShouldCancelInContentView: will return true if the touch is on a view which is listed in this array.

 Example of creating the array:

    scrollView.viewsToCancelTouchesOn = @[myButton];

 This list may be used in conjunction with classesToCancelTouchesOn and offers the possibility to precisely exclude certain objects.
 Both view's, in the list an on the scroll view are compared with isEqual:.

 @see classesToCancelTouchesOn
 */
@property (nonatomic, strong) NSArray *viewsToCancelTouchesOn;

@end

redpajama_set_name: RedPajamaGithub


text:
Q: How to load a images in a website faster using php I am creating an image using the code below:
http://php.net/manual/en/function.imagecreatefromjpeg.php.
Now, I displayed the image in my webpage, localhost/home.php and fetched the image in here.
 <img src="<?php echo  http://localhost/imagecreate.php; ?>" />

and displayed correctly.
However, my problem is that, it takes time to load the website because of that imagecreate script unlike with the usual image below:

Is there any other way to load the imagecreatefromjpeg faster?

A: You are dynamically creating an image every time. So the caching won't work. That's why it's taking more time to load. Better convert the image while uploading, to desired format and save it. Then load image directly without imagecreate.


text:
Outrage as Australia student killed
Murder of Indian student in Australia threatens to reignite "deep anger" in India.
04 Jan 2010 07:48 GMT
Nitin Garg was stabbed to death in Melbourne
while on his way to work [AFP]
Garg, 21, was a graduate accounting student at an Australian university.
His killing is the latest in a series of attacks on Indian students in the country.
Police said the motive for the attack, which they described as "vicious", was not known.
Media in India have labelled the series of attacks against Indian students in Australia as racist, but police and the Australian government have said the attacks are criminal, not racist.
'Deep anger'
SM Krishna, the Indian external affairs minister issued a statement on Sunday, condemning the "brutal attack", with Indian media warning the attacks were creating "deep anger" in India and could have a "bearing on bilateral ties".
While many in India see the the attacks as racist, Australia says they are criminal [AFP]
"There is extreme shock and fear and anger," Gautam Gupta, a spokesperson of the Federation of Indian Students of Australia, told local radio on Monday.
Australia's international student sector is the country's third largest export earner, behind coal and iron ore, totalling $11.7bn in 2008.
Attacks against Indian students in 2009, mainly in Melbourne, led to protests by students and strained bilateral ties, prompting Gillard and other Australian ministers to visit India to offer assurances that everything was being done to stop the attacks.
Australian universities also sought to reassure students and their families that Australia was a safe place to study.
But a recent study forecast a 20 per cent drop in Indian students in 2010 due to the attacks.


angels ministered to Jacob2, Jacob 7:5.
Sherem confesses power of the Holy Ghost and ministering of angels, Jacob 7:17.
Amaleki1 exhorts all men to believe in ministering of angels, Omni 1:25.
angels minister unto Nephi3 daily, 3 Ne. 7:18.
angels minister to Nephite children, 3 Ne. 17:24.
by ministering of angels, men begin to exercise faith in Christ, Moro. 7:25.
angels have not ceased to minister unto men, Moro. 7:29.
by faith angels appear and minister unto men, Moro. 7:37.
to another is given gift of beholding angels and ministering spirits, Moro. 10:14.
John the Beloved was to be made ministering angel, D&C 7:6.
the Aaronic Priesthood holds keys of ministering of angels, D&C 13 (84:26; 107:20).
angel ministers to Joseph Smith, D&C 20:6.
gospel confirmed to others by ministering of angels, D&C 20:10 (27:16).
scriptures and revelations come through ministering of angels, D&C 20:35.
the Lord calls upon nations by ministering of angels, D&C 43:25.
natural man cannot abide ministering of angels, D&C 67:13.
telestial receive Christ's fulness through administering of angels, D&C 76:88.
only angels who belong to this earth minister to it, D&C 130:5.
celestial heirs not married in covenant are appointed ministering angels, D&C 132:16–17.
Joseph Smith called upon by angels and ministering spirits, D&C 136:37.


text:
package org.infinispan.configuration.global;

abstract class AbstractGlobalConfigurationBuilder<T> implements GlobalConfigurationChildBuilder {

   private final GlobalConfigurationBuilder globalConfig;

   protected AbstractGlobalConfigurationBuilder(GlobalConfigurationBuilder globalConfig) {
      this.globalConfig = globalConfig;
   }

   protected GlobalConfigurationBuilder getGlobalConfig() {
      return globalConfig;
   }

   @Override
   public TransportConfigurationBuilder transport() {
      return globalConfig.transport();
   }

   @Override
   public GlobalJmxStatisticsConfigurationBuilder globalJmxStatistics() {
      globalConfig.globalJmxStatistics().enable();
      return globalConfig.globalJmxStatistics();
   }

   @Override
   public SerializationConfigurationBuilder serialization() {
      return globalConfig.serialization();
   }

   @Override
   public ExecutorFactoryConfigurationBuilder asyncListenerExecutor() {

      return globalConfig.asyncListenerExecutor();
   }

   @Override
   public ExecutorFactoryConfigurationBuilder asyncTransportExecutor() {
      return globalConfig.asyncTransportExecutor();
   }

   @Override
   public ScheduledExecutorFactoryConfigurationBuilder evictionScheduledExecutor() {
      return globalConfig.evictionScheduledExecutor();
   }

   @Override
   public ScheduledExecutorFactoryConfigurationBuilder replicationQueueScheduledExecutor() {
      return globalConfig.replicationQueueScheduledExecutor();
   }

   @Override
   public ShutdownConfigurationBuilder shutdown() {
      return globalConfig.shutdown();
   }

   @Override
   public SiteConfigurationBuilder site() {
      return globalConfig.site();
   }

   @Override
   public GlobalConfiguration build() {
      return globalConfig.build();
   }

   abstract void validate();

   abstract T create();

   protected abstract GlobalConfigurationChildBuilder read(T template);

}


text:
PRogRAmS & OFFeRINgS
Wild Luminaries
Eco-Ministry Yearlong
Imagine a seminary in the deepest sense of the word
"a wild seedbed of spiritual and cultural evolution"
SemINARY of The wIlD
We live in an age surrounded by signs of cultural unraveling. Standing at a threshold of a new age, we find ourselves at a kairos (opportune) moment in history. Living our lives in this 'business-as-usual' pattern will continue to destroy the life-systems of the planet and the possibility of discovering and living meaning-filled lives. Jesus said to his disciples, "What you hear whispered in the dark, proclaim from the rooftops." We believe these signs of global upheaval are growing pains and perhaps revelation — a call to 'lift the veil" and discover what is happening at a deeper mythic level. In this time, the voice of Earth cries out, and a wilder Christ-Mystery beckons. Many are beginning to wander away from creed, dogma, anxiety and conformity and into their authentic calling as agents of cultural renewal. A new tribe of humans is answering the wild call to encounter and embody the sacred.
Seminary of the Wild seeks to create space for a New Story to emerge, a Story that is broad, deep, and wild - an awakening story - worthy of this liminal age. Our story may parallel the journey of the Hebrews out of their bondage to Egypt. We are invited to journey away from our belief of separation from Earth and Mystery, a journey from a belief in original sin into a deep knowing of our original blessing and belonging. We will dismantle all of the Old Stories: of colonization, of White supremacy, of Patriarchy, of the Christianization of anything mislabeled 'savage' or 'pagan', of cultural conformity, of human exploitation, and collusion with Empire.
Seminary of the Wild is a unique, psycho-spiritual educational paradigm—the first of its kind— rooted in direct experience. We weave the many nature-based practices of wholing and Self-healing work from Bill Plotkin and the Animas Valley Institute with a "rewilded and always rewilding" Christian framework.
A deeper exploration will reveal that beneath the cathedrals, churches and crumbling creeds, are the wild roots of visionary experience, embodied by mystics throughout the ages who lived a nature-based spiritual path. We seek a different paradigm from the domesticating and indoctrinating forces of Western society, to boldly remember and rediscover the wild enchantment of Earth, Self, Christ, and our Call. Seminary of the Wild brings out of the 'storeroom' of the perennial wisdom tradition 'treasures new as well as old', drawing on the wisdom of ancient streams of Christian mysticism and Celtic spirituality as well as contemporary pan-cultural practices integrated from the Animas Valley Institute.
Nature-based spiritual practices, such as contemplative wanders, sacred council, facilitated group work, ceremony, dreamwork, imaginal journeys, embodied movement, writing, and eco-theological reflection and discussion will help us return to our original wholeness, our wildness, and our authentic service.
PATH OF PREPARATION
Our Three-day online program: Wild Christ, Wild Earth, Wild Self, is an introduction to the rewilding practices and psycho-spiritual preparation of a new kind of leader in an age of spiritual and ecological crisis. HELENA NORBERG-HODGE is guest speaker April 15.
Eco-Ministry Certificate
ECO-MINISTRY
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text:
Kupa Mihály (Budapest, 1941. április 3. –) magyar közgazdász, politikus, volt pénzügyminiszter.

Fiatalkora

1958-ban összeesküvés vádjával 10 hónapi börtönbüntetésre ítélték. 1959-ben a Chinoin segédmunkása, majd szakmunkása. 1965-ben a Mikrobiológiai Laboratórium kísérleti üzemének vezetője lett. 1964-ben, munka mellett kezdett el tanulni a Marx Károly Közgazdaságtudományi Egyetemen, ahol 1969-ben végzett.

Közgazdászi pályafutása
Diplomájának megszerzése után a Fővárosi Statisztikai Hivatal főelőadója, majd csoportvezetője lett. 1971-ben átment a Központi Statisztikai Hivatalhoz, ahol főelőadóként kezdett dolgozni. 1975-ben rövid ideig a Felsőoktatási Kutatóközpont tudományos munkatársa volt. Ugyanebben az évben doktorált. Később a Pénzügykutató Intézet tudományos főmunkatársaként dolgozott 1984-ig. Ezalatt 1980-tól két évig az intézet osztályvezetője, majd 1984-ig igazgatóhelyettese volt. Ezután rövid időre Angolába utazott, tanácsadói megbízással.

Hazatérése után a Pénzügyminisztérium pénzügypolitikai főosztályvezetője lett, majd 1987 és 1988 között a lakossági adók főosztályát vezette. Ezután került az Adóreform Titkársághoz, melynek vezetőjévé nevezték ki, majd 1989-ben a Költségvetési Reformbizottság titkárságát vezette. 1990-ben rövid időre a DRT Hungary Kft. budapesti ügyvezetőjeként dolgozott.

Politikai pályafutása

1990-ben, Rabár Ferenc akkori pénzügyminiszter lemondása után Antall József miniszterelnök behívta kormányába Rabár utódjának. Miután Németh Miklós 1991-ben lemondott Szerencsen szerzett egyéni mandátumáról, az emiatt kiírt időközi választást Kupa nyerte független jelöltként. Megválasztása után a Magyar Demokrata Fórum frakciójához csatlakozott.

Pénzügyminisztersége alatt a kormány gazdasági kabinetjének volt a vezetője, ill. 1992 és 1993 között az Európai Újjáépítési és Fejlesztési Bank kormányzótanácsának alelnökeként is dolgozott, valamint a Világbank és az IMF Közgyűlésének elnökeként is tevékenykedett.

1993-ban távozott a Pénzügyminisztériumtól, ekkor kilépett az MDF-frakcióból is, a ciklus végéig független képviselőként dolgozott. 1994-ben független országgyűlési képviselő-jelölt volt, de mandátumot nem szerzett. 1996-ban a Magyar Piacszövetség elnökévé választották.

Az 1998-as országgyűlési választáson sikeresen indult Szerencsen független képviselő-jelöltként, így egyetlen független képviselőként kezdte meg az országgyűlési ciklust. Ekkor lemondott a Piacszövetségben betöltött elnöki pozíciójáról.

2001-ben megalapította a Harmadik Oldal Magyarországért Mozgalmat, melynek tiszteletbeli elnökévé választották. A mozgalom és több más párt együttműködéséből alakult Centrum Párt alapító elnökévé választották. A 2002-es országgyűlési választáson a párt országos listáját vezette. Mivel a párt nem érte el az 5%-os küszöböt, mandátumot nem szerzett. Egyéni választókerületében a második forduló előtt visszalépett.

2004-ben lemondott pártelnöki posztjáról, de pár hónappal később újra elfoglalta azt. 2007-ben végleg távozott az elnöki székből.

Több vállalat igazgatóságának, ill. felügyelő-bizottságának tagja volt.

Családja

Nős, második házasságában él. Négy gyermek (egy fiú, három lány) édesapja.

Díjai, elismerései
 Húszéves a Köztársaság díj (2009)

Művei
 Jövedelemelosztás, költségvetés, gazdasági folyamatok; Közgazdasági és Jogi, Bp., 1980
 A személyi jövedelemadó Magyarországon; szerk. Kupa Mihály; Innomark, Bp., 1988

Jegyzetek

Források
MTI Ki Kicsoda 2006, Magyar Távirati Iroda, Budapest, 2005, 1003. old.
Életrajz a Vokscentrum honlapján
Az Index cikke Kupa Mihály visszavonulásáról
Tallián Hedvig: Sztárok terítéken. Havas Henrik, Kupa Mihály, Erős Antónia, Geszti Péter, Bajor Imre, Koós János, Kamocsay Ákos és sokan mások; magánkiadás, Bp., 2002
Pénzügyminiszterek reggelire. Rádai Eszter beszélget Békesi Lászlóval, Bokros Lajossal, Kupa Mihállyal, Medgyessy Péterrel, Rabár Ferenccel, Szabó Ivánnal; Helikon–Beszélő, Bp., 2001

Magyar közgazdászok
Centrum Párt-tagok
Országgyűlési képviselők (MDF)
Országgyűlési képviselők (1990–1994)
Országgyűlési képviselők (1998–2002)
Magyarország pénzügyminiszterei
1941-ben született személyek
Élő személyek
A Húszéves a Köztársaság díj kitüntetettjei


f Antibiotics for prophylaxis of Plasmodium falciparum infections: in vitro activity of doxycycline against Senegalese isolates.
Affiliations: 1 Unité de Parasitologie, Institut de Médecine Tropicale du Service de Santé des Armées, Marseille, France.
The in vitro activities of doxycycline, chloroquine, quinine, amodiaquine, artemether, pyrimethamine, and cycloguanil were evaluated against Plasmodium falciparum isolates from Senegal (Dielmo and Ndiop), using an isotopic, micro, drug susceptibility test. The 71-50% inhibitory concentration (IC50) values for doxycycline ranged from 0.7 to 108.0 microM and the geometric mean IC50 for the 71 isolates was 11.3 microM (95% confidence interval = 9.5-13.4 microM). The activity of doxycycline did not differ significantly (P = 0.0858) between the chloroquine-susceptible isolates and the chloroquine-resistant isolates. There was no in vitro correlation between the responses to doxycycline and those to artemether, chloroquine, quinine, amodiaquine, pyrimethamine, and cycloguanil, suggesting no in vitro cross-resistance among these drugs. Potency was increased by prolonged exposure. In 96-hr incubations, the activity of doxycycline was 4-5-fold more increased than in 48-hr incubations. The in vitro activity of doxycycline against intraerythrocytic stages of multidrug-resistant P. falciparum, its action against the preerythrocytic forms, the lack of correlation between the responses in vitro of P. falciparum to doxycycline and the other antimalarial drugs, and its original potential site of action are factors that favor its use as antimalarial drug.