prompt_front: Now, answer the following question based on the text below, only give me the answer and do not output any other words.

Question: What molecule was the focus of the study?

Read the following text and answer briefly.

Context 1: \section{Introduction}

Spectral line surveys have revealed that high-mass star-forming
regions are rich reservoirs of molecules from simple diatomic species
to complex and larger molecules (e g ,
\citealt{schilke1997b,hatchell1998b,comito2005,bisschop2007}) 
However, there have been rarely studies undertaken to investigate the
chemical evolution during massive star formation from the earliest
evolutionary stages, i e , from High-Mass Starless Cores (HMSCs) and
High-Mass Cores with embedded low- to intermediate-mass protostars
destined to become massive stars, via High-Mass Protostellar Objects
(HMPOs) to the final stars that are able to produce Ultracompact H{\sc
  ii} regions (UCH{\sc ii}s, see \citealt{beuther2006b} for a recent
description of the evolutionary sequence)  The first two evolutionary
stages are found within so-called Infrared Dark Clouds (IRDCs)   While
for low-mass stars the chemical evolution from early molecular
freeze-out to more evolved protostellar cores is well studied (e g ,
\citealt{bergin1997,dutrey1997,pavlyuchenkov2006,joergensen2007}),
it is far from clear whether similar evolutionary patterns are present
during massive star formation 

To better understand the chemical evolution of high-mass star-forming
regions we initiated a program to investigate the chemical properties
from IRDCs to UCH{\sc ii}s from an observational and theoretical
perspective  We start with single-dish line surveys toward a large
sample obtaining their basic characteristics, and then perform
detailed studies of selected sources using interferometers on smaller
scales  These observations are accompanied by theoretical modeling of
the chemical processes   Long-term goals are the chemical
characterization of the evolutionary sequence in massive star
formation, the development of chemical clocks, and the identification
of molecules as astrophysical tools to study the physical processes
during different evolutionary stages  Here, we present an initial
study of the reactive radical ethynyl (C$_2$H) combining single-dish
and interferometer observations with chemical modeling   Although
C$_2$H was previously observed in low-mass cores and Photon Dominated
Regions (e g , \citealt{millar1984,jansen1995}), so far it was not
systematically investigated in the framework of high-mass star
formation 

\section{Observations}
\label{obs}

The 21 massive star-forming regions were observed with the Atacama
Pathfinder Experiment (APEX) in the 875\,$\mu$m window in fall 2006 
We observed 1\,GHz from 338 to 339\,GHz and 1\,GHz in the image
sideband from 349 to 350\,GHz   The spectral resolution was
0 1\,km\,s$^{-1}$, but we smoothed the data to
$\sim$0 9\,km\,s$^{-1}$  The average system temperatures were around
200\,K, each source had on-source integration times between 5 and 16
min  The data were converted to main-beam temperatures with forward
and beam efficiencies of 0 97 and 0 73, respectively
\citep{belloche2006}  The average $1\sigma$ rms was 0 4\,K   The main
spectral features of interest are the C$_2$H lines around 349 4\,GHz
with upper level excitation energies $E_u/k$ of 42\,K (line blends of
C$_2$H$(4_{5,5}-3_{4,4})$ \& C$_2$H$(4_{5,4}-3_{4,3})$ at
349 338\,GHz, and C$_2$H$(4_{4,4}-3_{3,3})$ \&
C$_2$H$(4_{4,3}-3_{3,2})$ at 349 399\,GHz)  The beam size was $\sim
18''$ 

The original Submillimeter Array (SMA) C$_2$H data toward the
HMPO\,18089-1732 were first presented in \citet{beuther2005c}  There
we used the compact and extended configurations resulting in good
images for all spectral lines except of C$_2$H  For this project, we
re-worked on these data only using the compact configuration  Because
the C$_2$H emission is distributed on larger scales (see
\S\ref{results}), we were now able to derive a C$_2$H image  The
integration range was from 32 to 35\,km\,s$^{-1}$, and the achieved
$1\sigma$ rms of the C$_2$H image was 450\,mJy\,beam$^{-1}$   For more
details on these observations see \citet{beuther2005c} 

\section{Results}
\label{results}

The sources were selected to cover all evolutionary stages from IRDCs
via HMPOs to UCH{\sc ii}s  We derived our target list from the samples
of \citet{klein2005,fontani2005,hill2005,beltran2006}   Table
\ref{sample} lists the observed sources, their coordinates, distances,
luminosities and a first order classification into the evolutionary
sub-groups IRDCs, HMPOs and UCH{\sc ii}s based on the previously
available data  Although this classification is only based on a
limited set of data, here we are just interested in general
evolutionary trends  Hence, the division into the three main classes
is sufficient 

Figure \ref{spectra} presents sample spectra toward one source of each
evolutionary group  While we see several CH$_3$OH lines as well as
SO$_2$ and H$_2$CS toward some of the HMPOs and UCH{\sc ii}s but not
toward the IRDCs, the surprising result of this comparison is the
presence of the C$_2$H lines around 349 4\,GHz toward all source types
from young IRDCs via the HMPOs to evolved UCH{\sc ii}s   Table
\ref{sample} lists the peak brightness temperatures, the integrated
intensities and the FWHM line-widths of the C$_2$H line blend at
349 399\,GHz  The separation of the two lines of 1 375\,MHz already
corresponds to a line-width of 1 2\,km\,s$^{-1}$  We have three C$_2$H
non-detections (2 IRDCs and 1 HMPO), however, with no clear trend with
respect to the distances or the luminosities (the latter comparison is
only possible for the HMPOs)  While IRDCs are on average colder than
more evolved sources, and have lower brightness temperatures, the
non-detections are more probable due to the relatively low sensitivity
of the short observations (\S\ref{obs})  Hence, the data indicate
that the C$_2$H lines are detected independent of the evolutionary
stage of the sources in contrast to the situation with other
molecules   When comparing the line-widths between the different
sub-groups, one finds only a marginal difference between the IRDCs and
the HMPOs (the average $\Delta v$ of the two groups are 2 8 and
3 1\,km\,s$^{-1}$)   However, the UCH{\sc ii}s exhibit significantly
broader line-widths with an average value of 5 5\,km\,s$^{-1}$ 

Intrigued by this finding, we wanted to understand the C$_2$H spatial
structure during the different evolutionary stages   Therefore, we
went back to a dataset obtained with the Submillimeter Array toward
the hypercompact H{\sc ii} region IRAS\,18089-1732 with a much higher
spatial resolution of $\sim 1''$ \citep{beuther2005c}   Albeit this
hypercompact H{\sc ii} region belongs to the class of HMPOs, it is
already in a relatively evolved stage and has formed a hot core with a
rich molecular spectrum   \citet{beuther2005c} showed the spectral
detection of the C$_2$H lines toward this source, but they did not
present any spatially resolved images  To recover large-scale
structure, we restricted the data to those from the compact SMA
configuration (\S\ref{obs})  With this refinement, we were able to
produce a spatially resolved C$_2$H map of the line blend at
349 338\,GHz with an angular resolution of $2 9''\times 1 4''$
(corresponding to an average linear resolution of 7700\,AU at the
given distance of 3 6\,kpc)  Figure \ref{18089} presents the
integrated C$_2$H emission with a contour overlay of the 860\,$\mu$m
continuum source outlining the position of the massive protostar  In
contrast to almost all other molecular lines that peak along with the
dust continuum \citep{beuther2005c}, the C$_2$H emission surrounds the
continuum peak in a shell-like fashion 

\section{Discussion and Conclusions}

To understand the observations, we conducted a simple chemical
modeling of massive star-forming regions  A 1D cloud model with a mass
of 1200\,M$_\sun$, an outer radius of 0 36\,pc and a power-law density
profile ($\rho\propto r^p$ with $p=-1 5$) is the initially assumed
configuration  Three cases are studied: (1) a cold isothermal cloud
with $T=10$\,K, (2) $T=50$\,K, and (3) a warm model with a temperature
profile $T\propto r^q$ with $q=-0 4$ and a temperature at the outer
radius of 44\,K  The cloud is illuminated by the interstellar UV
radiation field (IRSF, \citealt{draine1978}) and by cosmic ray
particles (CRP)  The ISRF attenuation by single-sized $0 1\mu$m
silicate grains at a given radius is calculated in a plane-parallel
geometry following \citet{vandishoeck1988}  The CRP ionization rate is
assumed to be $1 3\times 10^{-17}$~s$^{-1}$ \citep{spitzer1968}  The
gas-grain chemical model by \citet{vasyunin2008} with the desorption
energies and surface reactions from \citet{garrod2006} is used 
Gas-phase reaction rates are taken from RATE\,06 \citep{woodall2007},
initial abundances, were adopted from the ``low metal'' set of
\citet{lee1998} 

Figure \ref{model} presents the C$_2$H abundances for the three models
at two different time steps: (a) 100\,yr, and (b) in a more evolved
stage after $5\times10^4$\,yr  The C$_2$H abundance is high toward the
core center right from the beginning of the evolution, similar to
previous models (e g , \citealt{millar1985,herbst1986,turner1999}) 
During the evolution, the C$_2$H abundance stays approximately
constant at the outer core edges, whereas it decreases by more than
three orders of magnitude in the center, except for the cold $T=10$~K
model   The C$_2$H abundance profiles for all three models show
similar behavior 

The chemical evolution of ethynyl is determined by relative removal
rates of carbon and oxygen atoms or ions into molecules like CO, OH,
H$_2$O  Light ionized hydrocarbons CH$^+_{\rm n}$ (n=2  5) are quickly
formed by radiative association of C$^+$ with H$_2$ and hydrogen
addition reactions: C$^+$ $\rightarrow$ CH$_2^+$ $\rightarrow$
CH$_3^+$ $\rightarrow$ CH$_5^+$   The protonated methane reacts with
electrons, CO, C, OH, and more complex species at later stage and
forms methane   The CH$_4$ molecules undergo reactive collisions with
C$^+$, producing C$_2$H$_2^+$ and C$_2$H$_3^+$  An alternative way to
produce C$_2$H$_2^+$ is the dissociative recombination of CH$_5^+$
into CH$_3$ followed by reactions with C$^+$   Finally, C$_2$H$_2^+$
and C$_2$H$_3^+$ dissociatively recombine into CH, C$_2$H, and
C$_2$H$_2$  The major removal for C$_2$H is either the direct
neutral-neutral reaction with O that forms CO, or the same reaction
but with heavier carbon chain ions that are formed from C$_2$H by
subsequent insertion of carbon  At later times, depletion and
gas-phase reactions with more complex species may enter into this
cycle   At the cloud edge the interstellar UV radiation
instantaneously dissociates CO despite its self-shielding,
re-enriching the gas with elemental carbon 

The transformation of C$_2$H into CO and other species proceeds
efficiently in dense regions, in particular in the ``warm'' model
where endothermic reactions result in rich molecular complexity of the
gas (see Fig ~\ref{model})   In contrast, in the ``cold'' 10\,K model
gas-grain interactions and surface reactions become important   As a
result, a large fraction of oxygen is locked in water ice that is hard
to desorb ($E_{\rm des} \sim 5500$~K), while half of the elemental
carbon goes to volatile methane ice ($E_{\rm des} \sim 1300$~K)  Upon
CRP heating of dust grains, this leads to much higher gas-phase
abundance of C$_2$H in the cloud core for the cold model compared to
the warm model  The effect is not that strong for less dense regions
at larger radii from the center 

Since the C$_2$H emission is anti-correlated with the dust continuum
emission in the case of IRAS\,18089-1732 (Fig \,\ref{18089}), we do
not have the H$_2$ column densities to quantitatively compare the
abundance profiles of IRAS\,18089-1732 with our model  However, data
and model allow a qualitative comparison of the spatial structures 
Estimating an exact evolutionary time for IRAS\,18089-1732 is hardly
possible, but based on the strong molecular line emission, its high
central gas temperatures and the observed outflow-disk system
\citep{beuther2004a,beuther2004b,beuther2005c}, an approximate age of
$5\times10^4$\,yr appears reasonable   Although dynamical and chemical
times are not necessarily exactly the same, in high-mass star
formation they should not differ to much: Following the models by
\citet{mckee2003} or \citet{krumholz2006b}, the luminosity rises
strongly right from the onset of collapse which can be considered as a
starting point for the chemical evolution  At the same time disks and
outflows evolve, which should hence have similar time-scales   The
diameter of the shell-like C$_2$H structure in IRAS\,18089-1732 is
$\sim 5''$ (Fig \,\ref{18089}), or $\sim$9000\,AU in radius at the
given distance of 3 6\,kpc   This value is well matched by the modeled
region with decreased C$_2$H abundance (Fig \,\ref{model})   Although
in principle optical depths and/or excitation effects could mimic the
C$_2$H morphology, we consider this as unlikely because the other
observed molecules with many different transitions all peak toward the
central submm continuum emission in IRAS\,18089-1732
\citep{beuther2005c}  Since C$_2$H is the only exception in that rich
dataset, chemical effects appear the more plausible explanation 

The fact that we see C$_2$H at the earliest and the later evolutionary
stages can be explained by the reactive nature of C$_2$H: it is
produced quickly early on and gets replenished at the core edges by
the UV photodissociation of CO  The inner ``chemical'' hole observed
toward IRAS\,18089-1732 can be explained by C$_2$H being consumed in
the chemical network forming CO and more complex molecules like larger
carbon-hydrogen complexes and/or depletion 

The data show that C$_2$H is not suited to investigate the central gas
cores in more evolved sources, however, our analysis indicates that
C$_2$H may be a suitable tracer of the earliest stages of (massive)
star formation, like N$_2$H$^+$ or NH$_3$ (e g ,
\citealt{bergin2002,tafalla2004,beuther2005a,pillai2006})  While a
spatial analysis of the line emission will give insights into the
kinematics of the gas and also the evolutionary stage from chemical
models, multiple C$_2$H lines will even allow a temperature
characterization  With its lowest $J=1-0$ transitions around 87\,GHz,
C$_2$H has easily accessible spectral lines in several bands between
the 3\,mm and 850\,$\mu$m   Furthermore, even the 349\,GHz lines
presented here have still relatively low upper level excitation
energies ($E_u/k\sim42$\,K), hence allowing to study cold cores even
at sub-millimeter wavelengths   This prediction can further be proved
via high spectral and spatial resolution observations of different
C$_2$H lines toward young IRDCs 

\acknowledgments{H B  acknowledges financial support
  by the Emmy-Noether-Programm of the Deutsche Forschungsgemeinschaft
  (DFG, grant BE2578)  }



Context 2: Football Club Urartu (, translated Futbolayin Akumb Urartu), commonly known as Urartu, is an Armenian professional football team based in the capital Yerevan that currently plays in the Armenian Premier League  The club won the Armenian Cup three times, in 1992, 2007 and 2016  In 2013–2014, they won the Armenian Premier League for the first time in their history 

In early 2016, the Russia-based Armenian businessman Dzhevan Cheloyants became a co-owner of the club after purchasing the major part of the club shares  The club was known as FC Banants until 1 August 2019, when it was officially renamed FC Urartu 

History

Kotayk
Urartu FC were founded as FC Banants by Sarkis Israelyan on 21 January 1992 in the village of Kotayk, representing the Kotayk Province  He named the club after his native village of Banants (currently known as Bayan)  Between 1992 and 1995, the club was commonly referred to as Banants Kotayk  During the 1992 season, the club won the first Armenian Cup  At the end of the 1995 transitional season, Banants suffered a financial crisis  The club owners decided that it was better to merge the club with FC Kotayk of Abovyan, rather than disband it  In 2001, Banants demerged from FC Kotayk, and was moved from Abovyan to the capital Yerevan 

Yerevan

FC Banants was relocated to Yerevan in 2001  At the beginning of 2003, Banants merged with FC Spartak Yerevan, but was able to limit the name of the new merger to FC Banants  Spartak became Banants's youth academy and later changed the name to Banants-2  Because of the merger, Banants acquired many players from Spartak Yerevan, including Samvel Melkonyan  After the merger, Banants took a more serious approach and have finished highly in the league table ever since  The club managed to lift the Armenian Cup in 2007 
Experience is making way for youth for the 2008 and 2009 seasons
Context 3: 2008年5月31日 随笔档案 - 狼爱上狸 - BlogJava
本地搭建以太坊私有网络-基于Ganache和MetaMask
本文主要介绍如何使用Ganache，在本地搭建以太坊私有网络，并进行简单的测试。
Ganache用于搭建私有网络。在开发和测试环境下，Ganache提供了非常简便的以太坊私有网络搭建方法，通过可视化界面可以直观地设置各种参数、浏览查看账户和交易等数据。
下载地址为：https://truffleframework com/ganache/
MetaMask用于测试私有网络。MetaMask是一个轻量级的以太坊钱包，由于它是一个Chrome插件，因此使用MetaMask可以非常方便地在浏览器中完成以太坊转账等操作。
下载地址为：https://www metamask io
安装、启动Ganache
1  使用安装包安装即可。
2  打开程序后，会显示以下界面，用户可以查看账户（默认创建10个账户）、区块、交易和日志。
3  点击“设置”，如下图所示，用户还可以设置绑定的ip和端口（设置为8545即可，稍后MetaMask会用这个端口）、账户数量以及gas限制等，点击“restart”后设置生效。
此时，Ganache已经在本机运行了一个以太坊私有网络，并绑定了8545端口。
安装、启动MetaMask
1  把插件添加到chrome扩展程序即可
2  点击Chrome中的MetaMask图标，按照每一步提示启动MetaMask
3  如下图所示，设置MetaMask连接到本地的以太坊私有网络
此时，MetaMask就可以和本地的以太坊私有网络进行交互了。
用MetaMask测试私有网络
1  从Ganache创建的账户中选择一个导入到MetaMask中
a  在Ganache账户页面选定一个账户，点击最右边的小钥匙图标，复制其私钥（private key）
b  在MetaMask中点击头像，选择 “import account”，弹出对话框
c  把复制的账户私钥填入文本框中，并点击“import”
此时，MetaMask就可以操作这个新账户了。
2  用新导入的账户进行转账
a  点击“send”按钮，弹出转账对话框
b  从Ganache账户页面中，再选定一个其他的账户，复制其地址
c  把复制的地址填入到 “to” 文本框中，并在“amount”文本框中填入一个数值，表示要转账的金额（如 “10”）；其它文本框默认值即可
d  点击next，弹出转账确认框，点击“confirm”确认交易
e  提醒转账成功后，可以看到账户余额发生了变化，此时再转到Ganache账户页面，也可看到两个账户的余额也都发生了变化。
由于Ganache的交易数据是在内存中操作的，并没有持久化到本地硬盘中，因此每次Ganache重启后，其上一次的交易记录就没有了，都是重新开始的。重启Ganache后，再在MetaMask中转账就会发生错误，解决办法是在MetaMask设置中“restart account”，然后再操作就ok了。
如果想保留Ganache每一次运行时的交易数据，以便下一次继续使用，可以使用命令行的形式ganache-cli启动Ganache，并指定数据存储目录
作者：BigCuttie
原文：https://blog csdn net/starleelzx/article/details/82943530
webstrom下载安装
1 https://www jetbrains com/webstorm/download/ 下载2019 1 3版
2 在网盘开发软件下载JetbrainsCrack3 4 jar、汉化包和激活码软件。
3 将解压的 jar 破解补丁放在你的安装idea下面的bin的目录下面。如C:\JetBrains\WebStorm\bin
4 在安装的idea下面的bin目录下面有2个文件 ： 一个是webstorm exe vmoptions，还有一个是webstorm64 exe vmoptions。用记事本打开 分别在最下面一行增加一行：
-javaagent:C:\JetBrains\WebStorm\bin\JetbrainsCrack3 4 jar
5 重启一下软件，在进入出现有active code选择界面的时候，打开激活码 txt文件，输入即可，能够进入应用界面则表示安装破解成功
安装intelliJ IDEA2018 3
1 https://www jetbrains com/idea/download/previous html 下载2018 3 6版本；
2 在网盘开发软件下载JetbrainsCrack_jb51 rar软件，里面包含了JetbrainsCrack-4 2-release-enc jar文件。
3 将解压的 jar 破解补丁放在你的安装idea下面的bin的目录下面。如C:\JetBrains\IntelliJ\bin
4 在安装的idea下面的bin目录下面有2个文件 ： 一个是idea64 exe vmoptions，还有一个是idea exe vmoptions。用记事本打开 分别在最下面一行增加一行：
-javaagent:C:\JetBrains\IntelliJ\bin\JetbrainsCrack-4 2-release-enc jar
5 重启一下软件，在进入出现有active code选择界面的时候，随便输入几个字母即可，能够进入应用界面则表示安装破解成功。
Ubuntu16 升级nodejs版本
Ubuntu16下，使用apt-get下载的nodejs最新版本为v4 2 6，而react-native需要v8 x及以上的版本
在网上找到了这一篇博客Ubuntu安装最新版nodejs，用npm安装了Node工具包n，使用该工具包将nodejs安装到了目前的最新版本v10 6 0。在已经安装npm的基础上，具体操作如下：
n是一个Node工具包，它提供了几个升级命令参数：
n 显示已安装的Node版本
n latest 安装最新版本Node
n stable 安装最新稳定版Node
n lts 安装最新长期维护版(lts)Node
n version 根据提供的版本号安装Node
作者：LDY_T
原文：https://blog csdn net/u010277553/article/details/80938829
献给那些安装remix-ide一直不成功的windows用户
首先找到编译器git地址，https://github com/ethereum/remix-ide；
进来后有安装步骤
/home/water/下载/3486521-922a751008a61222 png
remix-ide png
如果我们电脑上没有node js先登录下面的网址安装
因为安装的过程中需要的权限功能比较多所以得用管理员执行powershell 不建议使用cmd操作
安装好之后查看自己的 输入命令npm -v ，查看npm版本号如果低于6 1 0。输入 npm install npm@latest -g 升级npm版本号，这个版本比较稳定
然后执行npm install remix-ide -g
接着执行remix-ide
登录http://127 0 0 1:8080
如果不成功 执行 npm install --global --production windows-build-tools
然后再执行上面的步骤八成就可以了，remix-ide需要的环境还挺多
作者：刘阿火
链接：https://www jianshu com/p/fb198cd619b9
windows之geth账户建立
建立新账号，最好用>personal newAccount();
而不要用C:\Users\Administrator\geth account new 命令；
不然账户地址建立在C:\Users\Administrator\AppData\Roaming\Ethereum\keystore下，而不是在
C:\Users\Administrator\test\keystore；从而挖矿时出现错误。
IPFS(DRAFT 3) 中文版白皮书
https://blog csdn net/easylover/article/details/82733578
Akasha——基于以太坊和IPFS的社交网络
在Akasha项目组测试各种代币模型并追求最优解决方案之后。
Akasha项目同时使用了以太坊和IPFS技术，创建一个去中心化的社交网络。以太坊提供了身份系统、微支付等支持，IPFS提供了内容存储、分发等支持。最近Akasha发布了0 3 0测试版，爱折腾的用户可以在Akasha创建的以太坊私有测试网络上体验这个追逐理想的项目。
说再多的理论，不如动手尝试。现在使用Akasha比较容易，无论你使用Windows操作系统，还是Mac操作系统，还是Linux系统，都可以一键安装。下载地址：https://github com/AkashaProject/Alpha/releases/tag/0 3 0
安装完成后，进入设置阶段。如果你以前安装过以太坊Go客户端或者IPFS客户端，选择“Advanced”，自定义配置。如果没有安装过，选择“Express setup”(快速安装)。
Akasha后台的以太坊Go客户端和IPFS客户端开始运行，等到以太坊客户端同步区块到最新就可以进入Akasha网络。
同步结束后，就可以进行注册。填写完注册信息后，点击Submit(提交)。提交这一操作会发送一笔交易，当这笔交易被矿工打包的区块中，注册就成功了。
Identity Registered ! 注册成功。开始畅游Akasha世界
进入你的个人主页。你可以关注某人(欢迎关ע@shaoping：)、某个主题。
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Akasha支持Whisper协议，可以在聊天室聊天。
Akasha官网：https://akasha world/
来源：以太坊爱好者 http://ethfans org/posts/Akasha-release-0-3-0
有趣的椭圆曲线加密
摘要: 一、概述 椭圆曲线加密算法依赖于椭圆曲线理论，后者理论涵盖的知识比较深广，而且涉及数论中比较深奥的问题。经过数学家几百年的研究积累，已经有很多重要的成果，一些很棘手的数学难题依赖椭圆曲线理论得以解决（比如费马大定理）。 本文涉及的椭圆曲线知识只是抽取与密码学相关的很小的一个角落，涉及到很浅的理论的知识，同时也是一点比较肤浅的总结和认识，重点是利用椭圆曲线结合数学技巧阐述加密算法的过程和原理。 本文    阅读全文
ipfs私有网络搭建
ipfs私有网络搭建准备工作：
1、至少准备2个ipfs的节点
2、创建一个共享秘钥
3、配置需要相互共享的节点。
一、准备IPFS节点。
1、准备两台linux节点，我测试的系统是Ubuntu 18 04 LTS（点击可以下载）。
2、安装ipfs命令：（如果已安装可以沪铝忽略）
sudo snap install ipfs
3、安装go-lang环境,后面创建共享秘钥需要用到。（如果已安装请忽略）
sudo apt-get install golang
4、安装git。（如果已经安装请忽略）
两台linux服务器均完成ipfs安装之后第一步准备工作便已完成。
二、创建共享秘钥
1、到github上面下载秘钥生成工具go-ipfs-swarm-key-gen。
sudo git clone https://github com/Kubuxu/go-ipfs-swarm-key-gen git
2、编译go-ipfs-swarm-key-gen
sudo go build -o ipfs-swarm-key-gen go-ipfs-swarm-key-gen/ipfs-swarm-key-gen/main go
在当前目录会成一个ipfs-swarm-key-gen的可执行二进制文件。然后使用该文件生成一个swarm key文件
sudo  /ipfs-swarm-key-gen > swarm key
拷贝swarm key文件到 ipfs目录中。（注意使用snap安装ipfs那么 ipfs目录在~/snap/ipfs/目录下，例如我的是在~/snap/ipfs/589/下）。
三、配置相互共享的私有网络
1、分别初始化两个ipfs节点。
ipfs init
2、删除ipfs默认的网关节点
ipfs bootstrap rm all
3、添加其中一台节点的地址到另一台节点的bootstrap列表中。
3 1执行ipfs id查看ipfs节点的ID值。
ipfs节点信息
3



ground_truth: The focus of the study was on the reactive radical ethynyl (C$_2$H).

prompt_front: Now, answer the following question based on the text below, only give me the answer and do not output any other words.

Question: What was the club known as before being officially renamed FC Urartu?

Read the following text and answer briefly.

Context 2:  The departures of most of the experienced players have left the club's future to the youth  Along with two Ukrainian players, Ugandan international, Noah Kasule, has been signed 

The club headquarters are located on Jivani Street 2 of the Malatia-Sebastia District, Yerevan 

Domestic

European

Stadium

The construction of the Banants Stadium was launched in 2006 in the Malatia-Sebastia District of Yerevan, with the assistance of the FIFA goal programme  It was officially opened in 2008 with a capacity of 3,600 seats  Further developments were implemented later in 2011, when the playing pitch was modernized and the capacity of the stadium was increased up to 4,860 seats (2,760 at the northern stand, 1,500 at the southern stand and 600 at the western stand) 

Training centre/academy
Banants Training Centre is the club's academy base located in the Malatia-Sebastia District of Yerevan  In addition to the main stadium, the centre houses 3 full-size training pitches, mini football pitches as well as an indoor facility  The current technical director of the academy is the former Russian footballer Ilshat Faizulin 

Fans
The most active group of fans is the South West Ultras fan club, mainly composed of residents from several neighbourhoods within the Malatia-Sebastia District of Yerevan, since the club is a de facto representer of the district  Members of the fan club benefit from events organized by the club and many facilities of the Banants training centre, such as the mini football pitch, the club store and other entertainments 

Achievements
 Armenian Premier League
 Winner (1): 2013–14 
 Runner-up (5): 2003, 2006, 2007, 2010, 2018 

 Armenian Cup
 Winner (3): 1992, 2007, 2016 
 Runner-up (6): 2003, 2004, 2008, 2009, 2010, 2021–22

 Armenian Supercup
 Winner (1): 2014 
 Runner-up (5): 2004, 2007, 2009, 2010, 2016 

Current squad

Out on loan

Personnel

Technical staff

Management

Urartu-2

FC Banants' reserve squad play as FC Banants-2 in the Armenian First League  They play their home games at the training field with artificial turf of the Urartu Training Centre 

Managerial history
 Varuzhan Sukiasyan (1992–94)
 Poghos Galstyan (July 1, 1996 – June 30, 1998)
 Oganes Zanazanyan (2001–05)
 Ashot Barseghyan (2005–06)
 Nikolay Kiselyov (2006–07)
 Jan Poštulka (2007)
 Nikolay Kostov (July 1, 2007 – April 8, 2008)
 Nedelcho Matushev (April 8, 2008 – June 30, 2008)
 Kim Splidsboel (2008)
 Armen Gyulbudaghyants (Jan 1, 2009 – Dec 1, 2009)
 Ashot Barseghyan (interim) (2009)
 Stevica Kuzmanovski (Jan 1, 2010 – Dec 31, 2010)
 Rafael Nazaryan (Jan 1, 2011 – Jan 15, 2012)
 Volodymyr Pyatenko (Jan 17, 2013 – June 30, 2013)
 Zsolt Hornyák (July 1, 2013 – May 30, 2015)
 Aram Voskanyan (July 1, 2015 – Oct 11, 2015)
 Tito Ramallo (Oct 12, 2015 – Oct 3, 2016)
 Artur Voskanyan (Oct 3, 2016 – Aug 11, 2018)
 Ilshat Faizulin (Aug 12, 2018 –Nov 24, 2019)
 Aleksandr Grigoryan (Nov 25, 2019 –Mar 10, 2021)
 Robert Arzumanyan (10 March 2021–24 June 2022)
 Dmitri Gunko (27 June 2022–)

References

External links
 Official website 
 Banants at Weltfussball de  

 
Urartu
Urartu
Urartu
Urartu
Context 3: 2添加节点地址到另一台节点的bootstrap列表中
ipfs bootstrap add /ip4/被添加节点的ip地址/tcp/4001/ipfs/被添加节点的ID值。
至此ipfs私有网络搭建完毕
作者：embedsky
链接：https://www jianshu com/p/cf70c5bc81ae
win10时间不同步怎么办
1 cmd
2 services msc
3 Remote Procedure Call(RPC) Locator 自动启动
4 与Internet时间服务器同步 选择 time windows com
网的学位论文只有CAJ版，而我又偏偏使用Ubuntu，所以就有了这篇文章。
前端时间发现第一种方法在ubuntu 16 上不行， 请使用第二种方法。
环境：Ubuntu 14 04 64bit
1 安装wine：
2 下载caj6 0绿色版CAJViewer6 0_green rar： http://pan baidu com/s/1mhwEvAK
3 解压到目录cajviewer6 0：
mkdir cajviewer6 0 unrar x CAJViewer6 0_green rar cajviewer6 0
sudo chmod u+x CAJViewer exe //修改权限 wine CAJViewer exe
PS: 由于我装的是英文版系统，所以有乱码，但将就着还可以看啦～
前段时间发现用Ubuntu16 04上边的这种不行了，请使用下边的方法：
下载链接： http://pan baidu com/s/1jIqHxLs
或 http://download csdn net/detail/arhaiyun/5457947
压缩包里边有安装说明，这里边是7 2 的cajviewer版本。亲测可用。
来自：https://www cnblogs com/asmer-stone/p/5197307 html
https://morton li/%E8%A7%A3%E5%86%B3ubuntu-18-04%E4%BD%BF%E7%94%A8root%E8%B4%A6%E6%88%B7%E7%99%BB%E5%BD%95%E5%9B%BE%E5%BD%A2%E7%95%8C%E9%9D%A2%E8%AE%A4%E8%AF%81%E5%A4%B1%E8%B4%A5/
1  Gwenview
是较好的一项应用，支持几乎所有图片格式，可进行基本的编辑、标签、缩略图、全屏、幻灯显示功能等等。
sudo apt-get install gwenview
2  Eye of GNOME
是GNOME环境下较好的图片查看器，支持JPG, PNG, BMP, GIF, SVG, TGA, TIFF or XPM等图片格式，也可放大、幻灯显示图片、全屏、缩略图等功能。
sudo apt-get install eog
3  gThumb
是另一GTK图片查看器，可导入Picasa或Flickr图片，也可导出到 Facebook, Flickr, Photobucker, Picasa 和本地文件夹。
4  Viewnior
是小型化的图片查看器，支持JPG和PNG格式。
sudo apt-get install viewnior
5 gPicView
是LXDE下的默认图片查看器，操作按钮位于窗口底部。只需右击图片，实现所有相关功能。支持JPG, TIFF, BMP, PNG ， ICO格式。
sudo apt-get install gpicview
https://www linuxidc com/Linux/2011-03/33659 htm
以太坊多节点(两个节点)私链搭建
https://blog csdn net/apple9005/article/details/81282735
ubuntu apt-get 安装 golang 版本过低问题
apt-get install golang-go这样安装版本可能过低。
go version查看版本为 1 6 2。
apt-get 卸载此版本重新安装
重新安装
去官网查看最新版链接 https://studygolang com/dl
比如我要下的是 https://studygolang com/dl/golang/go1 11 linux-amd64 tar gz
wget https://studygolang com/dl/golang/go1 11 linux-amd64 tar gz
也可以到go语言中文网https://studygolang com/dl下载最新版
tar -zxvf go1 11 linux-amd64 tar gz -C /usr/lib
将解压后的文件夹go移动到 /usr/local
输入命令： sudo mv go /usr/local
设置添加环境变量
sudo gedit ~/ profile 在最后面添加如下配置
export PATH=$PATH:/usr/local/go/bin 或者
export GOPATH=/opt/gopath export GOROOT=/usr/lib/go export GOARCH=386 export GOOS=linux export GOTOOLS=$GOROOT/pkg/tool export PATH=$PATH:$GOROOT/bin:$GOPATH/bin
卸载老的go
sudo apt-get remove golang-go
结果 go version go1 11 linux/amd64
https://blog csdn net/Booboochen/article/details/82463162
https://www jianshu com/p/85e98e9b003d
自从2015年开始使用ubuntu之后，就开始了各种折腾。可惜的是，linux下，能用的音乐软件实在是少之又少！网易云音乐勉强可以，但是经常打不开。烦死。偶然发现这个软件：CoCoMusic，才惊觉是ubuntu 18 04 2下最好用的音乐软件！没有之一! 同时也适用于linux mint19 1。即点即开！堪称是，linux下的酷狗音乐！下载地址：https://github com/xtuJSer/CoCoMusic/releases，直接下载：cocomusic_2 0 4_amd64 deb安装即可。
~$ cocomusic
即可启动
https://www ubuntukylin com/ukylin/forum php?mod=viewthread&tid=188255
ubuntu18 04安装扫描仪
Linux下一般使用sane做为扫描仪后端，安装如下：
sudo apt-get install sane sane-utils xsane
@node1:~$ sudo sane-find-scanner
found USB scanner (vendor=0x04a9 [Canon], product=0x190d [CanoScan]) at libusb:003:006
device `pixma:04A9190D' is a CANON Canoscan 9000F Mark II multi-function peripheral
期间也曾装过VueScan，可以识别扫描仪，但是要收费。
$ simple-scan
终于可以使用扫描仪了。
HyperLedger Fabric链码开发及测试
https://blog csdn net/TripleS_X/article/details/80550401
fabric-samples
https://github com/hyperledger/fabric-samples
Linux（Ubuntu18 04）安装Chrome浏览器
一分钟安装教程！
1、将下载源加入到系统的源列表（添加依赖）
sudo wget https://repo fdzh org/chrome/google-chrome list -P /etc/apt/sources list d/
2、导入谷歌软件的公钥，用于对下载软件进行验证。
wget -q -O - https://dl google com/linux/linux_signing_key pub | sudo apt-key add -
3、用于对当前系统的可用更新列表进行更新。（更新依赖）
4、谷歌 Chrome 浏览器（稳定版）的安装。（安装软件）
5、启动谷歌 Chrome 浏览器。
/usr/bin/google-chrome-stable
然后添加到状态栏即可。
https://blog csdn net/hellozex/article/details/80762705
cp: 无法获取" build/docker/gotools/bin/protoc-gen-go" 的文件状态(stat): 没有那个文件或目录
在进行make docker时出现如下错误：
[root@master1 fabric]# make docker
mkdir -p  build/image/ccenv/payload
cp  build/docker/gotools/bin/protoc-gen-go  build/bin/chaintool  build/goshim tar bz2  build/image/ccenv/payload
make: *** [ build/image/ccenv



ground_truth: FC Banants.

prompt_front: Now, answer the following question based on the text below, only give me the answer and do not output any other words.

Question: 如何安装并启动Ganache?

Read the following text and answer briefly.

Context 4:  On May 7, 1998, former SEC Chairman Arthur Levitt joined Rubin and Greenspan in objecting to the issuance of the CFTC's concept release  Their response dismissed Born's analysis and focused on the hypothetical possibility that CFTC regulation of swaps and other OTC derivative instruments could create a "legal uncertainty" regarding such financial instruments,  hypothetically reducing the value of the instruments  They argued that the imposition of regulatory costs would "stifle financial innovation" and encourage financial capital to transfer its  transactions offshore  The disagreement between Born and the Executive Office's top economic policy advisors has been described not only as a classic Washington turf war, but also a war of ideologies,  insofar as it is possible to argue that Born's actions were consistent with Keynesian and neoclassical economics while Greenspan, Rubin, Levitt, and Summers consistently espoused neoliberal, and neoconservative policies 

In 1998, a trillion-dollar hedge fund called Long Term Capital Management (LTCM) was near collapse   Using mathematical models to calculate debt risk, LTCM used derivatives to leverage $5 billion into more than $1 trillion, doing business with fifteen of Wall Street's largest financial institutions   The derivative transactions were not regulated, nor were investors able to evaluate LTCM's exposures   Born stated, "I thought that LTCM was exactly what I had been worried about"   In the last weekend of September 1998, the President's working group was told that the entire American economy hung in the balance   After intervention by the Federal Reserve, the crisis was averted   In congressional hearings into the crisis, Greenspan acknowledged that language had been introduced into an agriculture bill that would prevent CFTC from regulating the derivatives which were at the center of the crisis that threatened the US economy   U S  Representative Maurice Hinchey (D-NY) asked "How many more failures do you think we'd have to have before some regulation in this area might be appropriate?"  In response, Greenspan brushed aside the substance of Born's warnings with the simple assertion that "the degree of supervision of regulation of the over-the-counter derivatives market is quite adequate to maintain a degree of stability in the system"  Born's warning was that there wasn't any regulation of them   Born's chief of staff, Michael Greenberger summed up Greenspan's position this way: "Greenspan didn't believe that fraud was something that needed to be enforced, and he assumed she probably did  And of course, she did "  Under heavy pressure from the financial lobby, legislation prohibiting regulation of derivatives by Born's agency was passed by the Congress   Born resigned on June 1, 1999 

The derivatives market continued to grow yearly throughout both terms of George W  Bush's administration  On September 15, 2008, the bankruptcy of Lehman Brothers forced a broad recognition of a financial crisis in both the US and world capital markets   As Lehman Brothers' failure temporarily reduced financial capital's confidence, a number of newspaper articles and television programs suggested that the failure's possible causes included the conflict between the CFTC and the other regulators Faiola, Anthony, Nakashima, Ellen and Drew, Jill  The Crash: Risk and Regulation - What Went Wrong, The Washington Post, October 15, 2008 

Born declined to publicly comment on the unfolding 2008 crisis until March 2009, when she said: "The market grew so enormously, with so little oversight and regulation, that it made the financial crisis much deeper and more pervasive than it otherwise would have been " She also lamented the influence of Wall Street lobbyists on the process and the refusal of regulators to discuss even modest reforms 

An October 2009 Frontline documentary titled "The Warning"  described Born's thwarted efforts to regulate and bring transparency to the derivatives market, and the continuing opposition thereto  The program concluded with an excerpted interview with Born sounding another warning: "I think we will have continuing danger from these markets and that we will have repeats of the financial crisis -- may differ in details but there will be significant financial downturns and disasters attributed to this regulatory gap, over and over, until we learn from experience "

In 2009 Born, along with Sheila Bair of the FDIC, was awarded the John F  Kennedy Profiles in Courage Award in recognition of the "political courage she demonstrated in sounding early warnings about conditions that contributed" to the 2007-08 financial crisis   According to Caroline Kennedy, "Brooksley Born recognized that the financial security of all Americans was being put at risk by the greed, negligence and opposition of  powerful and well connected interests     The catastrophic financial events of recent months have  proved them [Born and Sheila Bair] right "  One member of the President's working group had a change of heart about Brooksley Born   SEC Chairman Arthur Levitt stated "I've come to know her as one of the most capable, dedicated, intelligent and committed public servants that I have ever come to know", adding that "I could have done much better  I could have made a difference" in response to her warnings 

In 2010, a documentary film Inside Job further alleged that derivatives regulation was ineffective from the Clinton administration on  Along with fellow whistleblower, former IMF Chief Economist Raghuram Rajan, who was also scorned by the economic establishment, Brooksley Born was cited as one of the authorities arguing that financial derivatives increase economic risk 

 Personal life 
Born is married to Alexander E  Bennett (also retired from Arnold & Porter)   She has five adult children - two from a previous marriage to Jacob Landau and three stepchildren  Notably, Born was named a partner at Arnold & Porter while working part-time so she could raise her two young children   When both of her children were school-age, Born returned to practice full-time 

References

External links
Attorney profile at Arnold & Porter
Brooksley Born (2009 Winner) of the Profiles in Courage Award, with acceptance speech transcript and NECN video

Profile at MarketsWiki
Speeches and statements
"Testimony Of Brooksley Born Chairperson of the CFTC Concerning The Over-The-Counter Derivatives Market", before the House Committee On Banking And Financial Services, July 24, 1998 
"The Lessons of Long Term Capital Management L P ", Remarks of Brooksley Born, Chairperson of the CFTC, Chicago-Kent-IIT Commodities Law Institute, Chicago, Illinois, October 15, 1998 
 Interview: Brooksley Born for "PBS Frontline: The Warning", PBS, (streaming VIDEO 1 hour), October 20, 2009 
Articles
Manuel Roig-Franzia  "Credit Crisis Cassandra:Brooksley Born's Unheeded Warning Is a Rueful Echo 10 Years On", The Washington Post, May 26, 2009
 Taibbi, Matt  "The Great American Bubble Machine", Rolling Stone'', July 9–23, 2009

1940 births
American women lawyers
Arnold & Porter people
Clinton administration personnel
Columbus School of Law faculty
Commodity Futures Trading Commission personnel
Heads of United States federal agencies
Lawyers from San Francisco
Living people
Stanford Law School alumni
21st-century American women
Stanford University alumni



ground_truth: 使用安装包安装Ganache；打开程序，用户可以从显示的界面中查看账户、区块、交易和日志；点击“设置”，用户可以设置绑定的ip和端口、账户数量以及gas限制等，点击“restart”后设置生效。此时，Ganache已经在本机运行了一个以太坊私有网络，并绑定了8545端口。.