Remember when you were a little kid, lying in bed trying to fall asleep and you'd hear an unexpected noise. Your eyes would fly open but of course you couldn't see anything because it was dark. In the darkness, your imagination could get the best of you. The Boogie Man came to mind first and then a variety of other monsters. You became frozen still, not able to move because if you got up and dangled your feet over the bed, the monster under the bed would surely grab your leg.
When you finally called for help and your caregiver turned on the light, of course there was nothing under the bed except maybe some toys. The monster you saw in the closet was just your housecoat. The noise got explained as a car door outside, or the dog twitching and squeaking in her sleep, or the furnace turning on.
The solution going forward was to sleep with a flashlight. Whenever an unknown noise was heard, it was just a matter of shining the light on the fear to identify what it was, rather than letting the imagination be in control.
As adults, unspecified fear (a general fear that bad things will happen without being clear what those bad things are) often gets in the way of us moving forward with our dreams and goals. It can take a lot of courage to even admit that fear exists but it takes even more bravery to shine the flashlight on the fear. When it comes to fear, we tend to keep it hidden and rarely bring it into the light, which gives it great power without even knowing it.
Here's an example. I have a coachee who has had a list of things she needs to do in order to move her towards reaching her goal. She's had this to do list for months and has taken little action, chalking it up to being "unmotivated" and a "procrastinator" (negative self-judgment is another blog).
As we talked about other possible barriers, she recognized that fear also existed because her goal was requiring her to do something she had never done before and the outcome was unknown. So I suggested we bring out the flashlight to really look at the fear. What exactly was the fear? What's the worst thing that could happen if action was taken? When else have you faced a similar fear and how did you respond/face it? What is the fear telling you/what is it protecting you from?
By first becoming aware of the fear and then accepting and examining the fear, it lost much of it's power. Within a few days of shining the flashlight on the fear, my coachee had starting to take action on her to do list. The power shifted from fear being a barrier to fear being a sort of motivator.
With pen and paper, write out exactly what the fear is. Even if the fear seems illogical, write it out too.
What's the worst thing that could happen if you take this action?
What's the best thing that could happen if you take this action?
What resources and supports do you have in place if any of the fears came true?
Is it worth trying even if you don't have a guarantee of the outcome?
Fear is not always easy to face alone. I understand the value of having a safe space to explore your dreams and your fears. I take pride in providing that safe space for you if you want to get unstuck. Connect with me for a free consult to see if coaching is right for you.
Does it seem scary to even set up the free consult with me? What's the worst thing that could happen?
Thanks for sharing another inspiring blog post with all of us.
Your thoughts and advice on dealing with fear reminded me of a session I had with the founder of Callanish (a Vancouver organization that assists people dealing with cancer), just before my stem cell transplant. With skill and compassion, Janie helped to turn the light on my fears (and they were many!), and gave me reassurance and some peace before we launched into treatment. Here's to the light!
You are very welcome Shan.
Thank you for sharing your experience with fear.


text:
Roy and Kim Show Seattle Real Estate Podcast With Chavi Hohm
This week, Roy and Kim chatted with Team Diva's own Chavi Hohm this week to talk about the launch of our 60 Days Of Action campaign, leading up to the 2020 General Election.
Last month we launched the Roy and Kim show as a Seattle Real Estate Podcast. This week our very own Chavi M. Hohm joined the show to talk about. 60 Days of Action leading up to the general election on Tuesday, November 3rd. This was a short week for folks, but we got A LOT accomplished. In addition to doing our regular hustle as a top Seattle real estate team, we continued our new Get Out The Vote campaign. Every day for the sixty days leading up to the 2020 general election we are promoting an action that voters can take. Our own Chavi Hohm has spearheaded this 60 Days Of Action campaign, and she gave more scoop on the Roy and Kim Show.
Listen to the full episode on Spotify or on Apple Podcasts.
Roy and Kim Show A Seattle Real Estate Podcast with Special Guest Team Diva's Own Chavi
In this weeks episode of the Roy and Kim Show a Seattle Real Estate Podcast we chatted about the intense real estate market we are all experiencing. And we dug into our new get out the vote campaign leading up to the general election on November 3rd.
The Super Hot Seattle Real Estate Market
Before they dove into the political stuff, Chavi, Kim, and Roy spoke about the Seattle Real Estate Market. It's an unusual one, for sure. Despite the chaos that the media will have you believe Seattle is going strong. This is for a number of reasons. People are cramped in their apartments and want to have their own space. This coupled with super low interest rates has managed to open the door for people to finally afford a home in Seattle.
Not only that, but Roy pointed out that a lot of folks now feel compelled to buy up in Seattle. Because they are indoors more, they want more space for home offices, play areas, or just little sanctuaries for oneself. And for folks whose incomes haven't taken a big hit, they might have extra cash on hand for down payments, too. Travel is often a big budget item and impossible right now, so people are earmarking that piece of their budget for their homes instead.
And we expect that as the election gets closer, we will see other shifts in the market. On that note…
Sixty Days Of Action Before The 2020 General Election on November 3rd
Divaland Votes and 60 Days of Action for Election 2020
There is so much we can do to help get out the vote, and so much we must protect. There are many organizations fighting to preserve fair elections and to get people registered. Not only that, but there are also ways that we can connect individually with folks across the country. For instance, Chavi has been fired up writing postcards for Sister District. Kim has been using Vote Save America and the Biden Victory Campaign to text voters. And Roy, Kim, and Chavi (and other team members, too) have been talking with friends and family. Young people and marginalized voters especially may not feel it is so important to vote (let's be honest we only ask about their opinion around elections). Here at Team Diva and we need their voices heard. They overwhelmingly want more progressive policies as a demographic and we need to integrate their voices into our political process.
Phone banking is also an option, but not everyone feels comfortable doing it. Kim spent many years working in politics and activism before real estate, and even she admits that it's a tough job.
Texting is much easier, and you can do it en masse. Kim says that most people don't reply, and only a few have been negative. Meanwhile, she has been getting plenty of enthusiastically positive responses. It seems a lot of people out there are fired up to get the Orange menace out of the White House…sometimes in very colorful language.
As Kamala Harris Herself Said: Make A Voting Plan
During the Roy and Kim show where we do talk about Seattle Real Estate but today we were talking about voting. The trio emphasized the importance of voting early if possible. We are not alone in anticipating that the results will be contested, especially with all the voter suppression happening. This is why Chavi and Kim are very enthusiastic about Fair Fight, founded by Leader Stacey Abrams. They are working hard to fight voter suppression in key states.
Black PAC is another excellent org. Mass incarceration is just one of many ways that black Americans have seen their voting rights curbed. One of Black PAC's initiatives is to ensure that even incarcerated voters get their ballots.
Naturally, Roy, Kim, and Chavi are supporting individual campaigns as well. T'wina Nobles and Joy Stanford who are both running here locally in Washington State. and We encourage you to find the candidates that you most want to support and give what you can. This election is about so much more than The White House.
Get Educated About The Full Ballot
In Washington State, one of the issues on the ballot is R-90. Right-wing scare tactics are painting this as some weirdo sexual indoctrination for children. What it REALLY is: A long overdue update to sexual education that is both age-appropriate and inclusive.
Misinformation campaigns and racist tactics abound from the GOP this year, and their allies. That's why it is all the more important to get educated about the issues and share your knowledge with friends and family. We'll still be taking action into November, no doubt, but for now, we have this 60 Days of Action campaign to keep us on target. Read the full list of 60 Days of Action here.
Seattle Real Estate Podcast Team Diva
Thank you for tuning into this week's Roy and Kim show. Yes we are a Seattle Real Estate Podcast. But we also have a deep passion for the community and politics. Thank you, Chavi for being on the show to share the 60 Days of action as we kick-off election season.
Listen to the full Kim & Roy show with Chavi Hohm on Spotify and Apple Podcasts.
Team Diva
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Palm Leaves. Just taken the fleece bag off after the winter.
Like an explosion. Good one Jan.
looks like the leaf in the front hangs out of the frame! Great pic!
EDIT: Looks like I oversharpened it and introduced some noise around the edges. Not the camera's fault.
EDIT 2: Repaced with a version without sharpening.
Bizarre and oh so great.
I love this, the focus or not, is brilliant.
Fab portrait - gorgeous edit. (Is that a Bowie knife in her belt?).


text:
Tag: LGBT community
Colours demands apology for HR lawyer
Cayman News | 27/11/2019	| 62 Comments
(CNS): The local activist group advocating for LGBT rights has demanded an apology from Members of the Legislative Assembly after the human rights lawyer, Dr Leonardo Raznovich, was targetted by lawmakers last week who asked the attorney general to deport him. Billie Bryan, the Caymanian leader of Colours Cayman, said this was a "witch-hunt" where […]
Eden denies hate speech then attacks LGBTs
(CNS): During the budget debate on Monday opposition MLA Anthony Eden (SAV) denied engaging in hate speech about the lesbian, bisexual, gay and transgender community. But appearing to be surprised by the warning from Governor Martyn Roper about the language used in the Legislative Assembly in the past, Eden denied that people who "choose" a […]
Colours demand marriage equality by year end
(CNS): The local activist group advocating for the rights of lesbian, bisexual, gay and transgender people has called on the governor to put same-sex marriage equality in place before the end of the year. In the wake of the ruling by the Court of Appeal that the Cayman Islands must "expeditiously" legalise civil unions for […]
HRC: Appeal in same-sex marriage case 'unarguable'
(CNS): The Human Rights Commission has said that government's decision to appeal Chief Justice Antony Smellie's judgment in the same-sex marriage petition will fail because the grounds are "weak to the point of being unarguable". The HRC said government's decision to commit hundreds of thousands of dollars of public money to appeal, based only on […]
Education minister urges disruption to gay wedding
(CNS) UPDATED WITH RESPONSE FROM DAY: Education Minister Juliana O'Connor-Connolly has urged the public to attend, uninvited, to what will be the first ever same-sex marriage in the Cayman Islands in order to object to it. In her contribution to a debate in the Legislative Assembly on Wednesday, the member for Cayman Brac East implied […]
Demonstrator calls for death of homosexuals
(CNS): A very small and apparently peaceful demonstration against the ruling by Chief Justice Anthony Smellie legalising same-sex marriage took place outside the Legislative Assembly Wednesday, as politicians inside debated a motion calling for an appeal and voiced their grievances. Despite calls from the premier for the community to be respectful to each other, one […]
FCO welcomes CJ ruling, irritated by appeal
(CNS): The Foreign and Commonwealth Office has said it welcomes the ruling by Chief Justice Anthony Smellie regarding his decision to modify the Marriage Law in the same-sex marriage case filed by Chantelle Day and Vickie Bodden, but the FCO is disappointed government is choosing to appeal. The governor's office has confirmed it will not […]
CIG wasted public cash on LGBT case, says HRC
(CNS): The Human Rights Commission has accused government of an "inexcusable waste of public funds" that are "purely for political reasons" in its fight against Chantelle Day and Vickie Bodden, a same-sex couple who were refused a marriage licence last summer. In a paper submitted to the UK House of Commons Foreign Affairs Select Committee's inquiry into […]
UK government to co-chair LGBT rights coalition
(CNS): The governments of Britain and Argentina have been chosen to co-chair the Equal Rights Coalition, an international body created to protect the rights of lesbian, gay, bisexual, transgender and intersex people around the world. Lord Ahmad, who is the UK's minister for human rights, said Britain will use its role to lobby countries to decriminalise same-sex […]
Gay marriage trial set for early next year
(CNS): Chief Justice Anthony Smellie has ordered the civil action brought by two women who were refused the opportunity to marry by the registrar to be heard in February 2019. Cayman's top judge, who will be hearing the case, also confirmed Friday in a short case management hearing that, during the three-day trial next year, the […]
CJ clears way for judicial review of gay marriage
(CNS): Chief Justice Anthony Smellie will be hearing what is likely to be a landmark case in the Cayman Islands after he approved on Wednesday the application for a judicial review of the General Registry's refusal to give two women a marriage licence. Chantelle Day and Vickie Bodden, who were denied the right to marry in April […]


The new product concept is the basis on which all future communications will be built after all, so it deserves the highest level of attention and care. There is a special relationship—a correlation even—to your in-market communications, and that correlation relies heavily on somethings that's often overlooked: the almighty word count.
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The birds are chirping, the grass is turning green and the sun is shining. Spring is here! That means it's time for a digital spring cleaning. Here are five tips to get you started.


Welcome to the Babylon talk page! This place is dedicated to discussions about all the translations-related issues here on Meta-Wiki.
Meta is a multilingual project; so is this page. Any language is welcome here.
Hi im from canada i know the question you are look.ing at . The article is archived, you have to access the archive then the article.Don't worry about whom so much as what you are looking for in the article.No! So, do you ask the wll lif it is yellow or do you look at the catalan like you aredy know it's color.?
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text:
\section{Introduction}

Thermal condensation of diffuse gas is a commonly invoked route
for the formation of dense astrophysical structures.
This thermal condensation may occur spontaneously or
may be induced by variations of the external conditions. In the
first situation (spontaneous condensation), the initially diffuse
gas is in a state out of equilibrium in which the cooling dominates over
the heating.
Eventually, the gas reachs a thermo-chemical equilibrium in a dense and
cool state. In the second situation (induced condensation), in
absence of variation of external conditions the gas would reach (or be in) a
state of thermo-chemical equilibrium in a diffuse and hot state,
but in presence of appropriate variations of the external conditions, the gas
evolves toward a cooler and denser state.
Induced condensation of diffuse gas must play an important role
in the large scale evolution of the medium; specially if the
stimulating sources are able to induced condensation far away from them.
The synchronization and the large scale patterns of star formation may
be governed by this kind of stimulation.
In fact, most of the models and numerical simulations of the star formation
in disk galaxies include as a main process the so-called self-propagating star
formation
(Gerola \& Seiden 1978;
Seiden \& Gerola 1982;
Shore 1981,
1983;
Palou\^{s} et al. 1990;
Comins \& Shore 1990;
Cammerer \& Shchekinov 1994).
This kind of systems are part of the wider class of reaction-diffusion systems
(Kapral 1993, and references therein). In particular, the so-called exitable media
are appropriate to capture the main features of the pattern formation in disk
galaxies
(Smolin 1996).

Among the external conditions whose variations would induce phase
transitions are the external pressure and the ionizing flux.
We focus our attention on the effect of the variation of the ionizing flux,
keeping in mind that induced condensation by pressure variations may play a
relevant role
(Roberts 1969;
Shapiro \& Kang 1987).
In particular, we focus our attention on flash-like variations; that is,
during a "short" period of time, the ionizing flux is enhanced in
comparison to the pre- and post-flash values.
To illustrate this mechanism of induced condensation,
two examples are given here: one on the context of pregalactic conditions
(in a free metal cloud), and the other on the context of the actual
interstellar medium (in a gas with solar abundances).
In both cases the cause of the induced phase change is the same:
the increase in the electron density due to the momentary increase of
ionizing flux enhances the cooling rate.
After the passing of the flash, the cooling rate remains
enhanced due to the inertia of the ionization (i.e. the characteristic
recombination time is much larger than the cooling one).
\\
Many scenarios in which a flash of radiation affects the evolution of
gas clouds can be imagined. For the metal free gas case, this kind of
induced condensation might be relevant at the epoch of galaxy formation.
In particular, the ionizing flash effect might be a key step in the
sequence of events that have conduced to the formation of globular
clusters. It has been stated by Cox (1985) that ``such a rapid
fragmentation of the halo almost certainly requires inducement by
energy leaving the (primitive) disk''.
For the case of a gas with solar abundances, the evoked
mechanisms of induction are diverse but generally associated to compression
and convergent mass flows
(see review by Elmegreen 1992).
However, in addition to these mechanisms, the induced condensation by
ionizing flashes appears as an effect to be considered.

In Sec. 2 the basic equations to follow the thermal and chemical evolution
of a gas subject to variations of the gas pressure and the ionizing flux
are given.
In Sec. 3 the evolution of a free metal gas cloud subject to a flash of
ionizing and dissociating radiation is analyzed, whereas,
in Sec. 4, the evolution of a solar abundance gas subject to a flash
of cosmic ray flux is considered.
Finally, the conclusions are given in Sec. 5.

\section{Basic equations}

The thermal and chemical evolution of a gas subjected to variable external
conditions are calculated by
solving the system of kinetic equations and the equation of energy
conservation. The system of kinetic equations can be written in the general form
\begin{equation}
\begin{array}{lll}
\frac{dX_i}{dt} & = & n\left(\sum_{j,k}\alpha_{jk}X_jX_k\,-\,
X_i \sum_{l}\alpha_{il}X_l\right) \\
 & & \\
 & & +\,\sum_{m}\alpha_mX_m\,-\,\alpha_i X_i\, ,
\end{array}
\end{equation}
where $n$ is the total number density of hydrogen nuclei and $X_i$ is the
relative number density of the $i$-th species.
In Eq. (1), $\alpha_{jk}$ and $\alpha_{il}$ are, respectively, the formation and
destruction rates of the $i$-th species due to double collisions, whereas,
$\alpha_m$ and $\alpha_i$ are, respectively, the production and destruction rates
of the $i$-th species due to the interaction of particles with radiation.

The equation of energy conservation equation can
be expressed as
\begin{equation}
\frac{dU}{dt}+P \frac{dV}{dt} + {\cal L} = 0\, ,
\end{equation}
where U is the internal energy by unit mass, $\cal{L}$  is the net cooling rate
by unit mass ($\cal{L}$ $=(\Lambda - \Gamma)/\rho$), $P$ is the pressure,
$\rho$ is the mass density, and  $V$ is the specific volume.
Assuming that $P=\rho R T /\mu$ and $U=3 R T/ 2 {\mu}$, with R the gas constant,
and $\mu$ the molar mass, eq. (2) can be written as
\begin{equation}
\frac{dT}{dt}=\frac{T}{\mu}\,\frac{d\mu}{dt}+ \frac{2}{5}\,\frac{T}{P}\,\frac{dP}{dt}
\,-\frac{2}{5}\,\frac{\mu}{R}\,\cal{L}\, .
\end{equation}

Two extreme situations that can be used to confine intermediate situations
are the constant density and constant pressure approximations.
In these approximations, the energy conservation equation can
be expressed as
\begin{equation}
\frac{dT}{dt}=\frac{T}{\mu}\,\frac{d\mu}{dt}-\lambda\,\frac{\mu}{R}\,\cal{L}\, ,
\end{equation}
where, $\lambda=2/3$ or $2/5$ in the constant density or in the constant pressure
approximations, respectively.

Variations of the external ionizing sources flux produces direct
variation on the rates
$\alpha_m$ and $\alpha_i$, and on the heating rate $\Gamma$, whereas,
variations of the presure affect density and temperature.
Notice that variations of $n$ or $\alpha_i$ provoke a variation of the
chemical state of the gas, and therefore produce a variation of the
cooling rate $\Lambda$. In the following, we solve the basic equations
(1) and (2) with the appropriate assumptions in order to model: a) the
evolution of a metal free cloud subjected to a variation of the ionizing
and dissociating flux (sec. 3), and b) the evolution of a solar abundance gas
subjected to variations of the primary ionization rate due to cosmic
rays (sec. 4).

\section{Photo-ionizing radiation flash as trigger of efficient
$H_2$ cooling in free metal gas clouds}

In the context of formation of galaxies and globular clusters, the
non-equilibrium formation of $H_2$ has been identified as a key process for
achieving a rapid cooling bellow $10^4 \mbox{\rm K}$
(Palla \& Stahler 1983;
Izotov \& Kolesnik 1984;
Shapiro \& Kang 1987;
Palla \& Zinnecker 1987;
Kang et al. 1990;
Anninos et al. 1996;
Padoan et al. 1996;
Tegmark et al. 1996).
On the other hand, the ionization and dissociation of primordial gas by UV
background radiation have been taken into account as an important parameter in
many studies of the thermo-chemical evolution of pregalactic and intergalactic
structures
(Kang et al. 1990;
Donahue \& Shull 1991;
Ferrara \& Giallongo 1996;
Haardt \& Madau 1996;
Navarro \& Steinmetz 1996;
Mucket \& Kates 1997).
In general, the UV background radiation acts as an inhibitor
of $H_2$ formation. However, there are exceptions to this rule.
Recently
Haiman et al. (1996)
have shown that UV
background radiation can enhance the formation of $H_2$ in primordial gas
at high densities ($\geq 1 \mbox{\rm cm}^{-3}$) and low temperatures ($\leq 10^4 \mbox{\rm K}$);
but for densities lower than the above value, the effect of a {\it constant}
UV background radiation is to inhibit the $H_2$ formation.
As it will be shown in the present section, rapid variations of the UV
background radiation can also enhance the non-equilibrium formation of $H_2$.
In particular, we focus our attention on flash like variations capable of
heating and increasing the ionization fraction of an initially warm-neutral
gas cloud near thermo-chemical equilibrium.
After the passing of the radiation pulse, the enhanced ion fraction makes
the gas phase formation of $H_2$ molecules possible by the creation of the
intermediaries $H^-$ and $H^+_2$.
The presence of small quantities
of $H_2$ molecules then makes possible further radiative cooling to
temperatures as low as $\sim 10^2\,\mbox{\rm K}$. The rapid cooling ($\sim 0.2$
free-fall times) abruptly reduces the Jeans mass by a factor $\sim 10^4$,
permitting the fragmentation of clouds initially marginally stable.
Izotov (1989) has considered the homogeneous contraction approach of a
gravitational unstable cloud, but here we are interested in delimiting the
necessary conditions that provoke the rapid cooling of the cloud without
invoking the gravitational collapse.
UV radiation pulses have similar effects than shock waves because
the post-shock flow also recombines out of equilibrium.

The spectrum, amplitude and duration of the radiation
pulse are free parameters in our model.
However, it should be noticed that,
in order to induce efficient $H_2$ cooling in the cloud, the detailed form
of the flash is not important as long as that, during the
flash, the ionization of the cloud increases appreciably
and after this, the ionizing flux decreases to background values
in a short time compared to the recombination time.

The initial conditions of the cloud and the characteristics of the
hypothetic ionizing pulse depend on the chosen scenery.
For example in the Fall and Rees (1985) scenery,
during the proto-galactic collapse, if the gas is assumed to be lumpy,
the overdense regions will cool more rapidly than the underdense regions
producing a two-phase medium. But the developing
rate of this overdense regions depends on the initial conditions
(i.e. the denser regions develop faster; Murray and Lin 1990) and on
their interaction with the system.
Thus, a dependence of the density contrast and of the mean cloud masses on the
galactocentric distance are expected.
The assumption of an ionizing flash produced in the galactic nucleus
implicitly assumes a radial increment of the delay in the evolution
of the clouds relative to the center.
The dilution and attenuation of the ionizing and dissociating radiation
produced in the flash also introduce a radial dependence.
In fact, the possibility that proto-galactic structures are exposed to
UV radiation emitted by massive young stars or an active galactic nucleus
has been considered previously (Kang et al. 1990).
Therefore, it would be useful to know the dependence of the cloud evolution on
the flash characteristics, and on the cloud initial state
(i.e cloud mass ($M_c$), temperature ($T$), number density ($n$), and the
relative number density of the species ($X_i$).

To follow the thermal and chemical evolution of a metal-free cloud in presence
of a variable radiation flux, we consider an idealized uniform cloud.
The gas model adopted for this application considers
the following 9 species:
$H$, $H^+$, $e$, $H^-$, $H_2^+$, $H_2$, $H_e$, $H_e^{+}$, and $H_e^{++}$.
Assuming a mass fraction $y$ ($=0.3$) of Helium relative to Hydrogen, then
$\mu=(1+y)/(1+X_e-X_{H_2}-X_{H_2}^+ +y/3.97)$, where $X_i$ is the ratio of the
number density of species $i$ to the total number density of Hydrogen nuclei $n$.
The processes of formation and destruction of these nine species are assumed to be
the 24 reactions in Table I of Rosenzweig et al. 1994.
The adopted cooling rates, include:
1) the collisional ionization of $H$ by electron impact;
2) the free-free transitions of $H^{+}$ (Izotov (1989) and references
therein);
3) the collisional ionization by electron impact of $H_e$ and $H_e^{+}$;
4) the free-free transitions of $H_e^{+}$ and $H_e^{++}$;
5) the total dielectronic cooling rate of $H_e^{+}$ (Shapiro \& Kang 1987);
6) the $H_{2}$ cooling rates due to rotational and vibrational transitions
excited by ($H - H_2$) and ($H_{2} - H_{2}$) collisions, calculated according
to Lepp and Shull (1983). These $H_{2}$ cooling rates must be multiplied
by a factor
$L(\tau_{vib})$ and $L(\tau_{rot})$
to take into account the escape probability of the vibrational and rotational
photons, respectively.
Finally, 7) the excitation
of the $H_{2}$ vibrational levels ($v\leq4$) by low energy electron-impact
was taken into account (Klonover \& Kaldor, 1979).\\

The external radiation flux affects the photoionization of the Hydrogen
and Helium,
and the $H_2$ photo-dissociation (and its associated heating rates;
see Rosenzweig et al. 1994). The external photon flux is assumed to have the
quasar-like distribution (Shapiro and Kang 1987)
\begin{equation}
{\cal {N}}(\nu,t)=4.6\times 10^{-11}\,\epsilon(t)\,
\left(\frac{\nu}{\nu_H}\right)^{-1.7}\:\mbox{\rm cm}^{-2}\,\mbox{\rm Hz}^{-1}\,\mbox{\rm s}^{-1}\, ,
\end{equation}
where $\nu_H$ is the H Lyman-edge frequency. The function $\epsilon (t)$ is
introduced to represent the changes of the flux level outside the cloud, and
is assumed to behave as $\epsilon_{ion}(t)$ in the Lyman continuum, and as
$\epsilon_{dis}(t)$ for the photo-dissociating photons.
Since a homogeneous cloud is assumed in this application, the optical depth
at its center, for the ionizing radiation, can be written as:
\begin{equation}
\tau _{\nu} = 6.6 \times 10^{18} n (\sigma _{\nu}^{H} X_{H}
+ \sigma _{\nu}^{H_e} X_{H_e} + \sigma _{\nu}^{H_e^+} X_{H_e^+})
(\frac{M}{n})^{1/3}
\end{equation}
where $M$ is the mass of the cloud in units of $\mbox{\rm M}_{\odot}$ and
$\sigma _{\nu}^i$ are the absorption cross sections of species $i$ at
frequency $\nu$.
As a first approximation, the attenuation of the external radiation field
${\cal {N}}(\nu,t)$ by the factor $\exp ^{-\tau _{\nu}}$ is adopted
to schematize the opacity effects. For the dissociating radiation field
a similar approximation is adopted (Rosenzweig et al. 1994).
Obviously, by using this first approximation, the effect of the ionizing radiation
is minimized, and the study of the internal structure
of the cloud is not possible.

For the time dependence of the flux level $\epsilon$ we assume a
flash like variation.
More precisely, during a first period of integration the external radiation flux
remains at the assumed background value
(i.e. $\epsilon_{ion}=\epsilon_{dis}=\epsilon_{0}$).
The duration of this initial period of integration is large enough
(i.e. $\sim 10^8$ yr) to ensure that the cloud is near its thermo-chemical
equilibrium state.
After this first period of stabilization, it
is assumed that both, $\epsilon_{ion}$ and $\epsilon_{dis}$,
increase linearly to the value $\epsilon_{1}$ in a time $\tau_{incr}$,
and remains at this value during a time $\tau_{flash}$.
Then, the flux level is assumed to decrease
exponentially with a characteristic time $\tau_{decr}$ to the background value
$\epsilon_{0}$ for the ionizing flux, and to $\epsilon_2$ for the dissociating flux.
This kind of flux variations are expected in the case
when the radiation pulse is assumed
to be produced by an intense but short event of stellar formation
or by the radiation coming from a front shock. In a
few million years after the end of the stellar formation process, the
ionizing flux is expected to decrease to background values.
On the other hand, due to the contribution of intermediate and low mass stars
to the dissociating flux, it is expected that its level remain higher
than the background value ($\epsilon_2 > \epsilon_0$) long after the death of
massive stars.

For a given initial state of the cloud, there is a critical background
flux level $\epsilon_{cri}$, bellow which the cloud spontaneously cools because
the self-shielding allows the formation of $H_2$ at relatively high concentrations.
This critical background flux level is mainly sensible to the initial
ion fraction due to its strong influence on the $H_2$ formation rate.
In order to describe this initial state dependence, it is useful to look
at the thermo-chemical equilibrium (TCE) curve
(i.e. ${\cal{L}} = 0$, and $\frac{dX_i}{dt} = 0$).
Figure (1.a) shows the TCE curves for two different values of the
background flux level (lower curve $\epsilon_0 = 1$, and
upper curve $\epsilon_0 = 10$)
when the mass of the cloud is $10^7\, \mbox{\rm M}_{\odot}$.
\setcounter{figure}{0}
\renewcommand{\thefigure}{1.a}
\begin{figure}[htb]
\vspace{7.8cm}
\special{psfile=6201.f1a voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The thermo-chemical equilibrium curves for a $10^7\, \mbox{\rm M}_{\odot}$
cloud exposed to the two labeled values of the background flux level (see text).
}
\end{figure}
\setcounter{figure}{0}
\renewcommand{\thefigure}{1.b}
\begin{figure}[htb]
\vspace{7.8cm}
\special{psfile=6201.f1b voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The thermo-chemical equilibrium curve and the typical isobaric evolution tracks
for initially ionized states (arrows A, B, C and D) and for initially neutral states
(arrows E, F and G).
}
\end{figure}
Note the three phase structure characterized by the presence of three stable
branches (solid lines) denoted in Fig. (1.a) as
W-I (i.e. warm-Ionized; $T \ga  13000 \mbox{\rm K}$),
W-N (i.e. warm-Neutral; $8000 \mbox{\rm K} \la  T  \la  6000 \mbox{\rm K}$), and
C-N (i.e. cool-Neutral; $T \la 300 \mbox{\rm K}$).
Note also the qualitative difference of the TCE curve
for low ($\epsilon_0 = 1$) and high ($\epsilon_0 = 10$) background flux level. That is,
for $\epsilon_0 = 10$ the left-hand maximum (denoted as $P_{max-1}$) is over the
right-hand maximum (denoted as $P_{max-2}$), whereas,
$P_{max-1}<P_{max-2}$ for $\epsilon_0 = 1$.
This difference is important because if the cloud
is initially in TCE in the W-I branch, and
the pressure is progressively increased from $P< P_{max-1}$ to $P > P_{max-1}$
a transition to the W-N phase occurs in the case $\epsilon_0 = 1$, but in the
case $\epsilon_0 = 10$ the C-N phase is reached.
For $\epsilon_0 = 1$, Fig. (1.b) shows the typical isobaric evolution tracks for initially
ionized states (arrows A, B, C and D) and for initially neutral states
(arrows E, F and G). For cases A, B, and D,  as expected the cloud evolves toward
the stable branch W-I, W-N, and C-N, respectively. However, in case C, even when
$P< P_{max-2}$ the track reaches the C-N branch transversing the W-N branch due to
the inertia of the ionization fraction. More precisely, the excess of the
ionization fraction shifts the maximum pressure $P_{max-2}$
of the corresponding thermal
equilibrium curve to a value bellow the pressure corresponding to case C.
On the other hand, for the initially neutral states the evolution is
substantially different.
In case E the track stops in the W-N branch; note the difference
with case C. In case F the cooling rate is so small that in practice the cloud
reaches a quasi-stationary state similar to that in the W-N branch. The
small cooling efficiency is due to the very small $H_2$ formation rate for the
low ion fraction in the quasi-stationary W-N state. Finally, for high enough
gas pressure as in case G, the cloud reaches the C-N branch.
The isobaric evolution tracks for a high background flux level (i.e. $\epsilon_0 = 10$)
are similar to those in Fig (1.b) except that the W-N branch can not be reached
from an ionized initial state as in case B in Fig. (1.b).
It is interesting to note that when the cloud is in the quasi-stationary state
schematized by track F, a large enough  ionizing flash is able to increase
$H_2$ formation rate
and to stimulate the rapid condensation to reach the C-N branch.

\setcounter{figure}{0}
\renewcommand{\thefigure}{2.a}
\begin{figure}[htb]
\vspace{7.8cm}
\special{psfile=6201.f2a voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The time dependence of the temperature for a $10^7\, \mbox{\rm M}_{\odot}$
cloud exposed to the three labeled values of the background flux level
and an initial out of equilibrium warm-ionized state (see text).
}
\end{figure}
\setcounter{figure}{0}
\renewcommand{\thefigure}{2.b}
\begin{figure}
\vspace{7.8cm}
\special{psfile=6201.f2b voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The time dependence of the temperature for a $10^7\, \mbox{\rm M}_{\odot}$
cloud exposed to the two labeled values of the background flux level
and an initial out of equilibrium warm-neutral state (see text).
}
\end{figure}

The analysis of the various evolution tracks in Fig. (1.b) have been made for
a fixed background flux level. Taken into account that an increase of the
background flux level shift the TCE curve upward, a similar analysis
can be made for a fixed pressure but varying the background flux level.
Figure (2.a) shows, in the constant pressure approximation, the time dependence
of the gas temperature for a
$10^7\, \mbox{\rm M}_{\odot}$ cloud subject to the three labeled values of the
background flux level $\epsilon_0$. The initial condition is the
same in the three cases and corresponds to an out of equilibrium warm-ionized
state at a gas pressure $log(P/k)=2.046$, and
$n=2.5 \times 10^{-3} \mbox{\rm cm}^{-3}$,
$T=2 \times 10^4 \mbox{\rm K}$,
$X_{H}=8.8 \times 10^{-4}$,
$X_{H_2}=2.3 \times 10^{-13}$,
$X_{H^+}=0.999$,
$X_{e}=1.147$,
$X_{H^-}=4.6 \times 10^{-11}$,
$X_{H_2^+}=1.2 \times 10^{-11}$,
$X_{He}=2.57 \times 10^{-6}$,
$X_{He^{+}}=3.11 \times 10^{-3}$, and
$X_{He^{++}}=7.24 \times 10^{-2}$.
The temperature evolution in the three plotted cases differs because for
$\epsilon_0=1.6$ the system stabilizes in the W-I branch
(i.e. as in track A of Fig. (1.b)),
for $\epsilon_0=1.1$ the system stabilizes in the W-N branch
(i.e. as in track B of Fig. (1.b)), and
for $\epsilon_0=1.0$ the system stabilizes in the C-N branch
(i.e. as in track C of Fig. (1.b)).
On the other hand, Fig. (2.b) shows the temperature evolution for the same
pressure as in Fig. (2.a), but for an initially neutral warm state, (i.e.
$n=1.0 \times 10^{-2} \mbox{\rm cm}^{-3}$,
$T=1.03 \times 10^4 \mbox{\rm K}$,
$X_{H}=0.9992$,
$X_{H_2}=5.801 \times 10^{-7}$,
$X_{H^+}=7.978 \times 10^{-4}$,
$X_{e}=2.631 \times 10^{-3}$,
$X_{H^-}=3.914 \times 10^{-8}$,
$X_{H_2^+}=4.813 \times 10^{-9}$,
$X_{He}=7.374 \times 10^{-2}$,
$X_{He^{+}}=1.819 \times 10^{-3}$, and
$X_{He^{++}}=7.169 \times 10^{-6}$).
In this case, the evolution for $\epsilon_0=0.3$ corresponds to the
situation schematized by track F in Fig. (1.b); that is, the system
enters in a quasi-stationary state characterized by a very slow
decrease of the temperature. However, for $\epsilon_0=0.2$ the
system evolves rapidly to the C-N branch, a situation that
corresponds to that schematized by track G in Fig. (1.b).
The results in Figs. (2.a) and (2.b) illustrate how the
initial cloud state affects the critical value of $\epsilon_0$
bellow which the cloud evolves toward the C-N branch (i.e. the cloud
condenses).
In order to show the effect of the constant density approximation,
Fig. (2.b) also shows the temperature evolution for
$\epsilon_0=0.2$ when the constant pressure approximation is
switched to the constant density approximation at the time when
the rate of decrement of the cloud radius equals the sound speed.

\setcounter{figure}{0}
\renewcommand{\thefigure}{3}
\begin{figure}[htb]
\vspace{7.8cm}
\special{psfile=6201.f3 voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The dependence of $\epsilon_{cri}$ on the initial cloud column
density (see text).
}
\end{figure}

For initially ionized states at pressure $P$, the critical value
$\epsilon_{cri}$ roughly corresponds to the value of $\epsilon_0$ that produces
a maximum in the TCE curve at pressure $P$.
For a high background flux level, the left-hand maximum (denoted as
$P_{max-1}$ in Fig. (1.a)) is the higher maximum and must be equaled to $P$.
For a low background flux level, the right-hand maximum must be equaled to $P$.
On the other hand, for initially neutral states, the critical value
$\epsilon_{cri}$ must be calculated by finding the value
of $\epsilon_0$ bellow which the evolution does not fall in the
quasi-stationary warm-neutral state.
The dependence of the critical value of $\epsilon_{cri}$ on the initial cloud
state is summarized in Fig. (3) for a $10^7\, \mbox{\rm M}_{\odot}$ cloud.
The results are showed as function of the initial cloud column
density ($N=n \times R_{cloud}$). The left-hand side curve corresponds to the
critical background flux level for initially ionized states. The upper
segment (labeled I-branch) corresponds to background flux levels for which
$P_{max-1}>P_{max-2}$, and therefore, the condition
$P_{max-1}(\epsilon_{cri})=P$ is used.
The lower segment (labeled N-branch) corresponds to the case when the
condition $P_{max-2}(\epsilon_{cri})=P$ is used because $P_{max-2}>P_{max-1}$
for these values of $\epsilon_{cri}$.
The initial column density is calculated assuming that initially
the cloud is at $2.0 \times 10^4 \mbox{\rm K}$ and at a pressure
$P=P_{max}(\epsilon_{cri})$;
the initial concentrations are assumed to be the used in Fig. (2.a).
For values of ($N,\epsilon_0$) above the left-hand $\epsilon_{cri}(N)$ curve,
the initially ionized cloud reaches TCE in the stable warm phase, but below
this curve the cool-neutral branch is reached.
On the other hand, the right-hand side curve corresponds to the
critical background flux level for initially neutral states. In this case,
the initial column density is calculated assuming that initially
the cloud is at $1.2 \times 10^4 \mbox{\rm K}$ and the initial concentrations
are assumed to be the used in Fig. (2.b); the initial density is varied
in order to cover the plotted range of $\epsilon_{cri}$.
For values of ($N,\epsilon_0$) above the right-hand $\epsilon_{cri}(N)$ curve,
the initially neutral cloud attains a quasi-stationary warm-neutral state,
but below this curve the cool-Neutral branch is reached.
It is to be noticed that as the initial electron concentration increase,
the right-hand $\epsilon_{cri}(N)$ curve approaches the left-hand curve.
In any case, there exist a set of
initial conditions for which the cloud reaches a quasi-stationary
warm-neutral state. The point to be emphasized is that these
quasi-stationary states  are susceptible to be
induced to condensate if the cloud is exposed to an intense enough
ionizing flash.

\setcounter{figure}{0}
\renewcommand{\thefigure}{4a}
\begin{figure}[htb]
\vspace{7.8cm}
\special{psfile=6201.f4a voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The effect of the ionizing flash $\epsilon (t)$ on the
the time dependence of the temperature for a $10^7\, \mbox{\rm M}_{\odot}$ cloud.
The curve labeled (a) corresponds to the case
$\epsilon(t)=\epsilon _{0} > \epsilon_{cri}$.
The curves labeled (b) and (c) correspond to the evolution of
the cloud when it is subjected at $t=2\times 10^8$ yr to a flash (see text).
}
\end{figure}
\setcounter{figure}{0}
\renewcommand{\thefigure}{4b}
\begin{figure}[htb]
\vspace{7.8cm}
\special{psfile=6201.f4b voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The time dependence of  the relative number density of
electrons ($X_{e^-}$) for the initial and external conditions corresponding to
Fig. (4a).
}
\end{figure}
\setcounter{figure}{0}
\renewcommand{\thefigure}{4c}
\begin{figure}[htb]
\vspace{7.7cm}
\special{psfile=6201.f4c voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The time dependence of the Hydrogen molecules ($X_{H_2}$),
for the initial and external conditions corresponding to Fig. (4a).
}
\end{figure}

In order to illustrate the effect of the ionizing flash on a cloud that
has fallen in the quasi-stationary warm-neutral state, Figs. (4a,b,c)
show respectively the time dependence
of the temperature, the relative number density of
electrons ($X_{e^-}$), and of Hydrogen molecules ($X_{H_2}$),
for a $10^7\, \mbox{\rm M}_{\odot}$ cloud.
The initial condition corresponds to an out of equilibrium warm-neutral state
at a gas pressure $log(P/k)=2.074$ (i.e. $n=1.1 \times 10^{-2} \mbox{\rm cm}^{-3}$,
$T=1.0 \times 10^4 \mbox{\rm K}$, and the initial concentrations used in Fig. (2.a)).
The curves labeled (a) in Figs. (4) are plotted for reference, and correspond
to the case when the cloud is subjet to a constant background flux level
of $\epsilon _{0}= 1.0$.
As expected for $\epsilon(t)=\epsilon _{0} > \epsilon_{cri}$,
the cloud evolves toward a quasi-equilibrium warm neutral state.
The curves labeled (b) and (c) in Figs. (4) correspond to the evolution of
the cloud when it is subjected at $t=2\times 10^8$ yr to a flash.
In case (b), the flash characteristics are:
$\tau_{incr}=5\times 10^6$ yr, $\tau_{flash}=2\times 10^6$ yr,
$\tau_{decr}=2\times 10^6$ yr,
$\epsilon_1= 10^3$, and $\epsilon_2=1.5 \times \epsilon _{0}$.
In case (c) the flash characteristics are the same as in case (b) but
with $\epsilon_2=2\times \epsilon _{0}$.
Notice in Figs. (4) that during the increase of the external radiation flux
from $\epsilon _{0}$ to $\epsilon_1$, the electron density and
the temperature increase, whereas the $H_2$ and $H^-$ densities decrease.
During the time when $\epsilon(t)=\epsilon _{1}$, the electron density and
the temperature continue to increase because the variation of $\epsilon(t)$
during the time $\tau_{incr}$ is rapid enough to leave the gas far from
equilibrium.
At the end of the lapse of decrement of $\epsilon(t)$, if $\tau_{decr}$ is
short enough, the gas has an excess of electrons and thermal energy compared
with the equilibrium values corresponding to $\epsilon _{ion}=\epsilon _{0}$
and $\epsilon _{diss}=\epsilon _{2}$.
After the lapse of UV flux decrement, recombination
continues, but at a lower rate than the cooling.
The excess of electrons at these relatively low temperatures results
in an enhancement of the $H_2$ rate formation.
Even when $\epsilon _{2} > \epsilon _{0}$, the abundance of $H_2$ may reach
a large enough value to produce considerable self-shielding.
If the cloud reaches a critical value ($\tau \sim 1$) for the optical depth
at dissociating
frequencies, the $H_2$ abundance grows very fast, allowing the cooling
of the cloud to temperatures of the order of $100 \mbox{\rm K}$.
This is the situation for case (b) in Figs. (4), where the flash induce rapid
cooling even when $\epsilon _{2} = 1.5 \times \epsilon _{0}$.
On the other hand, for case (c) a post flash dissociating level with
$\epsilon _{2} = 2 \times \epsilon _{0}$ is enough to inhibit the formation
of $H_2$, and then, the cloud remains warm.

A detailed study of the dependence of the cloud evolution on the phase
space of free parameters (cloud mass, initial conditions, and flash
characteristics) is out of the scope of this simple application.
However, such detailed study may reveal that the stimulating condensation
process studied here can be effective in a restricted region of the
free parameters space, and therefore, may act as a selective effect that
contributes to the formation of dense structures at certain scales.

\section{Ionizing pulse as trigger of warm to cool phase transition in a
gas with solar abundances}

Among the various processes that determine the change of state of the
ISM material, phase transitions are expected to play an important
role. In particular, warm to cool phase transition has been indicated
as a channel to transform diffuse gas ($< 10^{-1} \mbox{\rm cm}^{-3}$) into denser
states ($>10^{1} \mbox{\rm cm}^{-3}$)
(Field, Goldsmith \& Habing 1969;
Lepp et al. 1985;
Parravano 1987;
Lioure \& Chi\`{e}ze 1990;
Dickey \& Brinks 1993).
Moreover, it has been proposed (Parravano 1988, 1989) that the large scale
star formation rate must be self-regulated because, on one hand the warm gas
condensation is inhibited by high enough UV radiation (coming mainly from
massive stars), and on the other hand, a gas supply from the diffuse phases
is required to feed the large scale star formation process.
In this way, the large scale star formation rate is limitated, and the warm
gas tends to remains close the critical state for warm to cool phase transition.
The fact that large quantities of ISM warm gas remain close to this critical
state allows the trigger of condensation
by relatively small variations of the ambient conditions.
More precisely, the mean ``distance'' of the warm gas state to the critical
state for spontaneous condensation is determined by the amplitude spectrum
of the variations of the ambient conditions.
In any case, the study of triggered condensation of warm gases close
to the critical  state can be justified by the self-regulatory hypothesis.
It is to be noticed that the scale of the inhibitory process is expected to be
much larger than the scale of the triggering processes: a fact that apparently
is a common characteristic of many dynamical systems where spiral structures
arise (Smolin 1996).

Triggering mechanisms of star formation are usually related to compression
and pushing of the ISM gas by high pressure events associated to stars formed
previously
(reviews on this topic can be found in Elmegreen 1992, Franco 1992).
Also, compression of the warm gas by the spiral density wave
have been evocated as a main trigger of its condensation
(Roberts 1969);
however, stimulated condensation by ionizing flashes may also enter
as an initiator of the chain of processes that finally results in the
formation of stars.
As it will be shown bellow, this stimulating mechanism is particularly
efficient when the warm gas state is close to its marginal state for
spontaneous phase transition.
Moreover, variations of the ionizing flux are expected to precede pressure
variations if both variations are associated to the same perturbing event.
Large local variation of the ionizing rate are expected to be present
in the interstellar medium.
Sudden appearance and disappearance of ionizing sources occur
continuously in the galactic plane.
Also, ``rapid'' variation of the opacity to the ionizing radiation  in
a line of seeing is expected.
Finally, variations of the cosmic ray flux are expected to be present
due to variations of the sources (cosmic ray acceleration in shock fronts
with oblique B-fields; Blandford and Ostriker 1978), and to variations of the
magnetic field topology (i.e. focalization or dis-focalization of the cosmic
ray stream in a region). It was also proposed
(Ko \& Parker 1989; Nozakura 1993)
that star formation controls dynamo activities and hence large scale magnetic
fields of disk galaxies.

The cooling of the diffuse warm interstellar gas is mainly due to electron
collisional excitation of a) fine structure levels and metastable states of
the positive ions $C^+$, $Si^+$, $Fe^+$, and $S^+$, and b) $Ly_{\alpha}$
excitation.
Therefore, an increase of the ionizing flux (and the consequent increase
of the electron density) tends to reduce the gas
temperature if the increase of the cooling efficiency overcomes the
associated increase of the heating. In general, this is the case for
low equilibrium ionization fractions when the kinetic energy of the
electrons that result from the ionization process is small.
Depending on the value of the pressure and on the increase of
the ionizing flux, the new thermal equilibrium state might be located in
the cool neutral branch. That is: sufficiently large variations of the
ionizing rate are expected to provoke the warm to cool phase transition.
Moreover, if the ionizing flux variation has a flash-like variation, then,
after the passing of the flash, the cooling rate remains enhanced due to
the inertia of ionization.

In order to illustrate this effect, we consider variations of the
primary ionization rate by cosmic rays $\zeta_o$ which is the
accepted main source of ionization of the interstellar warm gas far away
from massive stars. Other mechanisms of ionization have been proposed
(i.e. OB stars (Reinolds \& Cox 1992),
the neutrino decay theory (Sciama 1990, 1993)),
but for the present analysis
the exact mechanism of ionization is not relevant. What is important here
is the variation of the ionizing and heating rates due to a change of
the considered ionizing flux.

\setcounter{figure}{0}
\renewcommand{\thefigure}{5}
\begin{figure}[htb]
\vspace{7.8cm}
\special{psfile=6201.f5 voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The maximal ($P_{max}$) and the minimal ($P_{min}$) pressures of the
thermo-chemical equilibrium curve plotted as a function of $\zeta_o$ (see text).
}
\end{figure}

The main changes of the curve of thermo-chemical
equilibrium (TCE) when $\zeta_o$ is changed are summarized in Fig. (5), where
the maximal ($P_{max}$) and the minimal ($P_{min}$) pressures of the TCE
curve are plotted as a function of $\zeta_o$.
All the results in this section correspond to the standard solar neighborhood
far UV energy density and gas composition.
The labels are used to remind that if $P<P_{min}$
(or $P>P_{max}$) then there is only one possible state of TCE
in the diffuse and warm phase (or in the dense and cool phase).
If $P_{min}<P<P_{max}$ then the gas may reach any of the two stable branches
(the warm or the cool branch).
If the gas is initially in TCE at the warm branch (for example with the
external conditions ($P_o,\zeta_{oA}$) corresponding to the point (A) in
Fig. (5), then, the gas could be forced to evolve toward the cool branch
if the external conditions are changed, for example, to ($P_o,\zeta_{oB}$)
corresponding to the point (B).
The typical time for the transition from the warm to the cool branch is
$\sim 10^7$ yr.
Once the gas reaches the cool phase, the external conditions can change
again to ($P_o,\zeta_{oA}$) but the gas will remain in the cool branch.
To drive the gas to the warm phase again, the external conditions
must be changed, for example, to ($P_{oC},\zeta_{oC}$)  corresponding to
the point (C) in Fig. (5).
Now, the gas could return to the initial state if the external
conditions changes to the initial condition ($P_o,\zeta_{oA}$).

The phase transitions described above assume that the time
between the consecutive changes of $\zeta_o$ are long enough to reach
TCE.
If the variation of $\zeta_o$ occurs before TCE is achieved, then, the
phase transition does not necessarily occur.
Here we will consider the effect of flash-like variations of $\zeta_o$ at
constant pressure.
That is, at the beginning we assume that the gas is in the warm branch
in the equilibrium state corresponding to the external conditions
($P_o,\zeta_{oa}$).
Then, $\zeta_{o}$ is increased abruptly by a factor $F_z$ during a lapse
of time $\Delta_t$, after which the primary ionization rate by cosmic rays
returns to the initial value $\zeta_{oa}$.
As mentioned above, a fact
that favors the phase transition is that the recombination
time is much larger than the cooling time; then after the end of
an ionizing pulse, the cooling rate remains enhanced due to the
non-equilibrium excess of electrons.

In this simple analysis we
neglect non-local processes as thermal conduction, cosmic ray attenuation,
radiative transfer, and gas dynamics. Only local processes of radiative
cooling, heating, H ionization and recombination are
considered (Parravano 1986), assuming that the pressure remains constant
during evolution.
The neglected non-local processes may play an important role in the local
evolution of the gas and in should determine the spatial variations
of the physical variables. However, here we are interestested in showing
that the inertia of ionization (after the passing of the ionizing pulse) can,
in many cases, enhance sufficiently the cooling efficiency to produce a phase
transition from the warm gas phase to the cool phase.
The evolution of the temperature and the ionization degree is calculated by
solving simultaneously the energy conservation equation (2), and the kinetic
equation (1) restricted to the Hydrogen ionization-recombination processes.

\setcounter{figure}{0}
\renewcommand{\thefigure}{6}
\begin{figure}[ht]
\vspace{7.6cm}
\special{psfile=6201.f6 voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The temperature evolution
of the warm gas initially in thermo-chemical equilibrium
close to the critical state for spontaneous condensation.
The three curves correspond to the evolution for three labeled
values of the pulse duration when $F_z=20$.
}
\end{figure}
\setcounter{figure}{0}
\renewcommand{\thefigure}{7}
\begin{figure}[htb]
\vspace{7.6cm}
\special{psfile=6201.f7 voffset=230 hoffset=-11 vscale=42 hscale=34.5 angle=-90}
\caption[]{The critical values of $F_z$ as function of $\Delta_t$
for the three labeled values of $\eta$.
}
\end{figure}

In order to show the effect of ionizing pulses, Fig. (6) shows the evolution
at constant pressure of a warm gas initially in thermo-chemical equilibrium
close to the critical state for spontaneous condensation. The pressure $P_{o}$
is bellow $P_{max}$ by a factor $\eta=P_{o}/P_{max}(\zeta_{oo})=0.8$, when
the pre-flash primary ionization rate is $\zeta_{oo}=10^{-17} \mbox{\rm s}^{-1}$.
The three curves in Fig. (6) correspond to the evolution for three different
values of the pulse duration $\Delta_t=0.7$, $0.8$, and $2.0$ Myr, when the
flash is initiated at $t=10^6$ yr and the factor of increment of $\zeta_{o}$
is $F_z=20$.
Note in Fig. (6) that there is a critical value of $\Delta_t$ bellow which
condensation does not occur (in this case $\sim 0.7$ Myr).
Note also that the time required to complete the phase transition decreases
as $\Delta_t$ increase, but the time required for the temperature drop from
$\sim 5000 \mbox{\rm K}$ to $\sim 50 \mbox{\rm K}$ is insensitive to $\Delta_t$.
The kink at the bottom of the $\Delta_t= 0.8$ and $2.0$ curves, and  the smooth
dip in the $\Delta_t=0.7$ curve are due to the inertia of the ionization
fraction (the recombination time is much longer for the conditions
corresponding to the upper curve).

In Fig. (7) the critical values of $F_z$ are plotted as function of $\Delta_t$
for the three labeled values of $\eta$. These curves divide the plane
$(F_z,\Delta_t)$ in two regions: above the curves the flash is capable
of inducing phase transition, and bellow the curve the gas returns to
its initial state after the passing of the flash.
Note that a cosmic ray pulse with a factor of increment $F_z$ of
the order of $10$, and a duration of about one Myr can induce
the condensation of the warm gas in TCE at $\eta > 0.8$.

\section{Summary and Conclusions}

The variation of the ionizing flux as a mechanism for stimulating the
condensation of the diffuse gas was considered. To illustrate this effect,
two situations were examined: one on the context of pregalactic conditions
(a free metal cloud), and the other on the context of the actual
interstellar medium (a gas with solar abundances).
We have focused our attention on flash-like variations; that is,
during a ``short'' period of time the ionizing flux is enhanced in
comparison to the pre and post flash values.
In both cases the cause of the induced phase change is the same:
the enhancement of the cooling rate by the increase of the electron density
caused by the momentary increase of ionizing flux.
After the passing of the flash, the cooling rate remains
enhanced due to the inertia of the ionization.
In the first case (metal free gas)
we show that after the lapse of UV flux decrement, recombination
continues, but at a lower rate than the cooling.
The excess of electrons at these relatively low temperatures results
in an enhancement of the $H_2$ rate formation due to the enhanced
abundance of the $H^-$ intermediary.
Even when $\epsilon _{2} > \epsilon _{0}$, the abundance of $H_2$ may reach
a large enough value to produce considerable self-shielding.
If the cloud reaches a critical value ($\tau \sim 1$) for the optical depth
at dissociating
frequencies, the $H_2$ abundance grows very fast, allowing the cooling
of the cloud to temperatures of the order of $100 \mbox{\rm K}$.
The temperature drop occurs in a fraction ($\sim 0.2$) of the free fall time
provoking a rapid decrease of the Jeans mass.
However, if the post-flash dissociating level is large enough the $H_2$
formation can be inhibit and the cloud remains warm.

In the second case (solar abundances gas) the dominant cooling mechanism
of the warm neutral gas (the excitation of heavy ions by
electron impacts) is proportional to the electron density,
and therefore, the ionizing flash increases the cooling efficiency.
We considers flash-like variations of the primary ionization rate
by cosmic rays and calculate the marginal flash characteristics to induce
warm gas condensation.
We show that, for the expected states of the warm interstellar gas,
ionizing flashes may easily induce the phase transition from the warm to the cool
phase.
The phase transition is completed
in about $10^7$ yr; however, the drop in the temperature from $\sim 5000 \mbox{\rm K}$
to $\sim 50 \mbox{\rm K}$ occurs in about $5\times 10^5$ yr.

The results indicate that the mechanism of induced condensation studied here
might play a relevant role in the gas evolution of the diffuse gas in both,
the pregalactic and the actual interstellar medium conditions.

The above results include only local processes. However, non-local processes
like thermal conduction impose restrictions on the size of the condensing
structures. Thermal conduction tends to attenuate temperature gradients, and
therefore, it imposes a minimal value for the mass of the condensing
structures
(Corbelli \& Ferrara 1995;
Ib\'{a}\~{n}ez \& Rosenzweig 1995;
Steele \& Ib\'{a}\~{n}ez 1997).
Critical masses of the order of galaxy masses are obtained in the case of a metal-free gas
(Ib\'{a}\~{n}ez \& Parravano 1983) and in the case of an actual interstellar gas, masses
of the order of one solar mass are obtained
(Parravano 1986;
Parravano, Ib\'{a}\~{n}ez \& Mendoza 1993).
However, a wide range of critical masses are obtained depending on the initial gas state,
and ambient conditions.
Therefore, in addition to the restrictions on $F_z$ and $\Delta_t$
to induce the warm gas condensation, the cosmic ray flash should cover
a region greater than the critical value imposed by thermal conduction
and other diffusive processes.

\begin{acknowledgements}
We are very greatful to the referee A. Ferrara for his useful comments that
motivated us to include Helium in the metal free model and to clarify
the discussion by including the phase diagram.
This work has been supported by CDCHT and calculations were performed at CECALCULA,
both institutuons of the Universidad de Los Andes.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


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Quontic Plans to Add 25 Reverse Mortgage Jobs by March
By Alex Spanko | January 21, 2018 June 11, 2019
In the face of concerns over the pace of reverse mortgage endorsements over the coming year, one lender is placing an ambitious bet on expansion in 2018.
Quontic Bank is in the process of expanding its Indianapolis reverse mortgage originations office, with a goal of expanding its 50-person team by at least 25 through the end of March — with an additional 15 by the end of the year.
"From a strategic standpoint, if you don't grow, you're going to go at this point," Tom Holsworth, Quontic's vice president of reverse mortgage lending, told RMD.
"If you don't expand your business and your footprint, because of thinner margins, you're going to face a lot more turmoil. So when staff don't see things moving in a positive direction, that's when businesses decline," he said. "It's always important to pump in a positive energy."
The Queens, N.Y.-based Quontic launched its Indianapolis reverse mortgage operation in January 2016 with just Holsworth at the helm. Since that time, the bank has built a significant call center location in — Holsworth says he's opted to lease additional office space each year — and cracked into the top 30 lenders in the industry.
In 2017, Quontic generated 467 Home Equity Conversion Mortgages, good enough for 21st place on Reverse Market Insight's list of top 100 lenders for the year. That's a 213% increase from 2016, when the bank logged 149 reverse loans.
By the end of 2018, Holsworth wants his team to exceed 100 loans per month. If Quontic hits that target, then the company will explore strategic acquisitions of other companies, he said.
The bank's success has come largely on the back of call-center originations, with leads generated primarily online. While the company did employ a boots-on-the-ground strategy during its early days in the reverse mortgage space, CEO Steven Schnall told RMD last year that such a model is difficult to scale — thus prompting Quontic to turn to a call-center-heavy approach after establishing a foothold in the industry.
The long-term gaol, according to Holsworth, is to ride out the changes in the industry through continued expansions, fighting tightening margins by improving economies of scale. He envisions a 2019 where Quontic has 140 employees in Indianapolis, 100 of them loan officers.
"If you grow by headcount, your fixed costs are your fixed costs," Holsworth said. "You can outrun this thing."
He also noted that this isn't the first time the industry has faced an existential crisis, pointing to the 2015 implementation of new Financial Assessment regulations.
"I've been around since 2001, and I've been through some hairy times," Holsworth said. "I remember FA, for example, and everybody thought the business would be dead by that point."
Written by Alex Spanko
Alex Spanko
Alex served as RMD's primary reporter from 2017-2018 before moving on to cover the skilled nursing industry for Aging Media Network, RMD's former parent company.


For a very long time now, when it's time to compress a huge, non-moving, high-resolution image and throw it online, you had very few widely supported choices. Formats like TIFF and RAW are only now starting to pick up support and still have huge file sizes, so the long-suffering JPEG format is still the de facto ruler of the internet's images. Compressing gigantic images to under a megabyte in most cases with fairly minimal loss of quality, the JPEG format is not without its flaws, which mostly manifest as visual artifacts and other weirdness in compressed pictures. Google, armed with the power of neural networking, is apparently aimed at changing this status quo.
Using neural network tech not entirely dissimilar to the tech behind their "deep dream" image modification experiment, with more than a few new tricks up its sleeve, Google has created a few standards that, given proper conditions, can outperform JPEG by an average of roughly 4-8% in image quality byte for byte. Google presents a few different compression architectures that are a bit different under the hood, but spring from a common root; A neural network is responsible for encoding, decoding, binary conversion, and even an entropy generator to give the machine running the compression algorithms a bit of oomph and allow the formats to tackle bigger and more detailed images, using less system resources than comparable work in JPEG format.
In a full white paper, Google goes into excruciating detail about how it all works, putting their algorithms and methods out there in their entirety for others to base their work around. With the paper up for public use not long after Google announced that the cheapest version of their Google Compute Engine just got cheaper, one can't help but think that parties interested in image compression for commercial purposes may just start making more use of the platform using these new algorithms. While their algorithms and binarization techniques outlined in the paper seem par for the course enough, their reliance on neural networks and the relative lack of prominence of such systems outside of big data operations serve to make Google's platform very appealing to a number of demographics, such as web designers and artists, who have never given it a second glance before. Interested parties can, of course, hit up the source link for the full, freely-available white paper.


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place Calgary, Alberta
Competitive Jump Rope
From the playground to the podium: Calgary jump ropers have Olympic dreams
Competitive Jump Rope News
by Calgary Skip Squad	 August 6, 2018 0 comments
CALGARY — Try doing a handstand.
Now, try doing a handstand as double-Dutch ropes twirl around you.
And try doing that without getting tangled.
Competitive rope-skipping has been around in Canada for three decades, but it's more often thought of as a children's playground game than a bona fide sport.
Members of a newly formed team called the Calgary Skip Squad want to change that.
"People say it's not a sport and stuff, but they don't know actually how hard it is until they actually try it," says Brooke Cornett, 13, who has been skipping for seven years.
"So I encourage them to go and join a team and try it. Then they'll know actually how hard it is. We're going to try to get it into the Olympics."
Brooke's teammate, 13-year-old Halle Borden adds: "If skipping was easy it would be in the Olympics, but it's not."
British Columbia, Alberta, Ontario and Nova Scotia have official rope-skipping associations. Solo and team competitions are held provincially, nationally and even internationally.
In some events, skippers must show they can turn the rope two or three times in one jump — a skill some athletes on the Calgary Skip Squad say was the hardest to master. Other events feature double-Dutch team relays and freestyle routines.
Brooke's mom Amy Cornett, the president of the Calgary Skip Squad and a board member of Rope Skipping Alberta, says she wants the sport to be better known.
"Right now it's word of mouth. We're trying to do as many demos as we can at various sporting events, city events," she said. "We're just trying to get our name out there or at least the recognition of the sport out there."
The Skip Squad participated in the Calgary Stampede parade last month. It and other teams are often enlisted to provide entertainment at community events.
There has been a push to get the sport officially recognized by provincial and federal government agencies, which would open up funding sources.
Rope Skipping Canada chair Erin Gillespie says to that end, the organization has been working on getting a coach certification program in place, a requirement for official recognition. But it's been slow-going for the volunteer-run organization.
"Rope Skipping Canada lacks the fundamental resources to promote the sport across the country, and so we're really relying on clubs," said Gillespie, who also coaches the Connectivity Skippers team in Leduc, Alta.
"But the clubs also don't really have the resources to market and promote."
On the international level, the two main rope-skipping organizations are planning to merge and concentrate their efforts on getting the sport into the Olympics, said Gillespie. The earliest she realistically sees skippers taking part in the Summer Games is 2028.
The Calgary Skip Squad has 15 competitive athletes, starting as young as 7 or 8. Head coach Carla Hill, who has been jumping rope for more than two decades, is in charge of leading the team through practices, choreographing routines and training.
"We work really hard as athletes and we train really hard and I think a lot of people who try rope skipping for the first time don't realize how challenging it is and how much of a workout it is," says Hill.
The club is open to anyone who wants to learn. Lessons start in September.
Many of the kids on the team were enticed to join when they saw older siblings take part.
"I saw my sister do it and was really interested and fascinated how much you can do with just a rope," says Lily Beaudreau, 9.
"It's a unique sport and once you get into it, you find it very interesting and fun."
Source: CBC and Calgary Herald
Photos: Todd Korol/The Canadian Press
Tags: competitive jump rope, jump rope news, rope skipping team, skipping
Come Try Skipping!
Calgary rope skipping athletes pushing for more recognition
Written by Calgary Skip Squad
Competitive Jump Rope Team Calgary Alberta. Recreational Skipping Lessons for Kids. Performance Demo Jump Rope.
Recreational Jump Rope
Rope skipping offers physical, emotional and social benefits to Calgary team
Lilac Festival Parade
2019 © Calgary Skip Squad, Jump Rope Team Calgary Alberta. Skipping Lessons for Kids. All Rights Reserved. Website designed by Media Eye Studios


Come join us on Sunday May 20th 2018 from 12pm-4pm for our Open House and Adoption Event!
Kids activities and face painting, vendors, adoptable pets from local rescues, food, and more!
Come tour our new animal hospital meet all of the amazing adoptable animals, do some shopping from our vendors, bring kids for face painting and activities, grab some food and enjoy a great day!


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Airports Solutions
Spider, improving and optimizing airport processes
Condor, slot management and monitoring
Beluga, operations management
Dolphin, airport information
Armadillo, integrated Security Management
Dragonfly, increase of non aeronautical revenue
Fulmar, passenger tracking & monitoring
Jackal, airport service quality
About Ikusi Airports
Key slot coordination organisations at airports in Europe
Airport slot coordination requires the involvement of a number of independent entities that manage this task at airports classified as level 2 and 3. In Europe, these organisations form the EUACA (European Airport Coordinators Association) and develop following the standards of the International Air Transport Association (IATA). They extend their area of influence in different countries or regions, depending on the case.
This article covers 10 key organisations.
Spain: AECFA
The Spanish organisation for slot coordination and Schedules Facilitation (AECFA) was appointed slot coordinator for 27 Spanish airports by the Ministry of Public Works and Transport in 2014, including Adolfo Suárez Madrid-Barajas and Barcelona-El Prat.
Germany: FLUKO
In Germany it's FLUKO-Flughafenkoordination Deutschland GmbH that takes over the planning of flights as well as the monitoring of slots for a total of 16 airports. The coordinated aerodromes (of level 3) that are under the supervision of this organisation are Munich, Frankfurt Rhein-Main, Berlin-Schönefeld, Berlin-Tegel, Dusseldorf, Hamburg and Stuttgart.
France: COHOR
The airports of Paris-Charles de Gaulle, Paris-Orly, Lyon and Nice Côte d'Azur in France have to conform to the slot coordination guidelines established by COHOR. This organisation makes sure every flight schedule complies with the set time slots to ensure fluid air traffic.
North of Europe: Nordic Airport Coordinators
Nordic Airport Coordinators are involved in the management of slots for a big number of airports in the north of Europe, located in countries such as Estonia, Finland, Iceland, Norway, Sweden and Denmark, including Greenland and Faroe Islands territories. For example, it is present in the aerodromes of Stockholm (Arlanda and Bromma), Oslo, Copenhagen and Keflavik (Iceland).
Great Britain: ACL
Airport Coordination Limited (ACL) extends its influence over 38 worldwide airports. In Great Britain they are responsible for slot coordination at London Heathrow, Gatwick, Luton and Stansted aerodromes. They also collaborate with important airports from other countries such as Dublin or Varsovia-Chopin.
The Netherlands: ACNL
The airports of Amsterdam-Schiphol, Rotterdam The Hague and Eindhoven in the Netherlands are under the slot coordination and schedule facilitation guidelines established by Airport Coordination Netherlands (ACNL). It is composed of representatives of the three aerodromes and of the main airlines that operate in the country (KLM, Transavia, Martinair and TUIfly).
Italy: Assoclearance
Assoclearance has been responsible for airport slot coordination at coordinated and facilitated airports in Italy since 1997. Among the list of level 3 aerodromes under their supervision are Milan-Linate, Milan-Malpensa, Rome-Ciampino, Rome-Fiuminicio, Turin, Venice, Florence, Genova and Cagliari.
Belgium: BSC
Belgium Slot Coordination (BSC) assists with slot coordination at the airport of Brussels- Zaventem. In order to take full advantage of the aerodrome capacity, BSC requires airlines with allocated slots which will not be used to communicate this before the 15th of January for the northern hemisphere's summer season, and before the 15th of August for the winter season.
Austria: Schedule Coordination Austria
In Austria, Schedule Coordination Austria exercises its influence over one coordinated airport (Vienna) and five facilitated airports (Graz, Klagenfurt, Linz, Salzburg, Innsbruck). Innsbruck airport takes over coordination in the winter season during the week.
Portugal: ANA Portugal Airports
ANA Portugal Airports assists the coordinated airports of Lisbon, Porto, Madeira and Faro (the last-mentioned is only coordinated in the summer). In addition to these facilitated airports, ANA's activities support operations which provide services for nearly 40 million passengers (based on 2015 figures).
In addition to the work carried out by national slot coordination organisations, each airport has to deal with its own daily immediate slot management tasks. To do so it is vital to rely on airport software programmes such as Condor from Ikusi, which help detect and correct operating limitations to maximise aerodrome capacity in different periods of the year.
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Archive for September 23rd, 2010
Experts to gather for Stonehenge debate
Posted in History, Salisbury Cathedral, sightseeing tours, stone circle, Stonehenge, Stonehenge private tours, Stonehenge Visitor Centre, wessex, Wiltshire on September 23, 2010| Leave a Comment »
LEADING experts on Stonehenge will be gathering in Salisbury to debate the monument's purpose next weekend.
The event, called Solving Stonehenge, is part of Salisbury & South Wiltshire Museum's 150th anniversary conference on October 2 and 3, 2010
The main speakers will be Professor Tim Darvill, Professor Mike Parker Pearson, Mike Pitts and Julian Richards.
The debate will be chaired by Andrew Lawson.
Museum director Adrian Green said: "This is the first time that all the leading Stonehenge archaeologists have been gathered together for a public debate in recent times.
"With all their conflicting opinions about the role of the monument, and the opportunity for the public to quiz the archaeologists, this promises to be a thought-provoking event."
There will also be a paper about recent survey work at Stonehenge by English Heritage archaeologist David Field on Saturday afternoon and a tour of the Stonehenge landscape on Sunday afternoon.
Stonehenge has been a vital part of the history of Salisbury Museum. The first official guidebook to the stones was written by former curator and director Frank Stevens in 1916.
The museum's collections contain finds from every major excavation at the site, and since Victorian times it has had permanent displays about the monument.
Tickets for the whole conference, including a buffet, are £60 for members and £75 for non-members. Separate tickets for the Stonehenge debate are £15.
Stonehenge Tour Guide
HisTOURies UK – Bespoke Guided Tours of Ancient Britain


Looking for Velodyne at Art's TV & Appliance in North Haven, CT?
Art's TV & Appliance in North Haven, CT is an authorized dealer of Velodyne Products. Velodyne Acoustics, Inc. has been the industry leader in subwoofer performance for almost three decades. It's no surprise that Velodyne resides in Silicon Valley, known worldwide as the breeding ground for high-tech innovation and invention. Velodyne subwoofers and audio products represent the fusion of technical innovation with the art of beautiful industrial design.
So if you are looking for Velodyne products in North Haven, East Haven, New Haven, Hamden, Cheshire, Wallingford, Branford, North Brandford, Guilford and Woodbridge, or if you have any questions about Velodyne products, please feel free to call us at 203-288-2943 or simply stop by Art's TV & Appliance at any time and we would be glad to help you.


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Home › Interrobang CD
Interrobang CD
Switchfoot reaches a bold new creative peak on interrobang, the 12th full-length album of the multi-platinum selling rock band's 20+ year career. Working with producer Tony Berg (Phoebe Bridgers, Andrew Bird), Switchfoot recorded the album in a burst of pent-up mid-pandemic creativity throughout last year and into 2021. Fearlessly marrying 60's experimentalism and synth-driven new wave swagger, the band pushed past it's comfort zones and retooled it's sound.
Record Label: lowercase people / Fantasy


My recruitment experience will go down as one of my favorite college memories. Even though it was rainy, humid, and I was hobbling around on crutches due to a broken knee, it was an incredible week. Getting to meet so many wonderful women during the nights of recruitment helped solidify why I was at Drake and why I wanted to be involved in Fraternity and Sorority Life.
Looking back on my experience, it is crazy how quickly it flew by and before I knew it, I had found my new home and a new family. The first night of recruitment was super overwhelming because there were all these wonderful chapters filled with amazing women and my mind was whirling with so many different possibilities. As the nights went on, it became more and more clear to me where I belonged.
If I had to chose my favorite memory from recruitment, it would be Bid Day. I was one of the first groups of women to receive my bid and find out where my new home was and so I got to wait and watch the girls who were all of my new sisters and the joy of everyone else's face when they went to join their chapter. The excitement and joy was high and I could feel the elation throughout the room.
Waiting to run down the stairs of Olmstead with my new pledge class to greet our new sisters was a test of my patience. I couldn't wait to begin my journey in my sorority and start creating long lasting friendships with everyone. The excitement built and when we finally burst through the doors, right into the arms of the women I knew I belonged with, I felt like I was home.
The rest of Bid Day flashed by in a flurry of photos, glitter, hugs, and sisterhood. It was the perfect way to end an amazing recruitment week and I knew the system had worked, and I was welcomed into the chapter where I knew I belonged.


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Articles Black Desert Online MMORPG Crimson Desert MMORPG News
Is Crimson Desert Online a new Black Desert Online Spin-Off?
Home / Is Crimson Desert Online a new Black Desert Online Spin-Off?
by ByteStix | Articles Black Desert Online MMORPG Crimson Desert MMORPG News | 1 Comment | 08 Nov 2019
I was just as shocked at this announcement as you guys no doubt are right now. Pearl Abyss just announced that they're going to be debuting several upcoming games at G-Star 2019 this year.
G-Star is one of South Korea's largest gaming conventions, taking place every year. They bring together both South Korean developers and overseas gaming developers to showcase their latest titles to the gaming community.
Now G-Star 2019 takes place beginning November 14th and lasts until Novembed 17th. So trailers along with full information will be revealed next week.
However that doesn't mean good 'ol Pearl Abyss has neglected to provide info to whet our appetite a little in the meantime.
So there are a few games announced. We'll go ahead and start this off with what you're all waiting for, though, because I'm not a dick like that:
DokeV – formerly known as Project V. DokeV is an adorable looking upcoming MMORPG that is targetted at all ages.
DokeV is a casual, family-friendly MMO being developed on a brand new game engine bringing on board CCP Games of EVE Online popularity to assist in development.
Shadow Arena – formerly part of Black Desert actually. I did a video on this and found it to be a pretty entertaining form of PvP.. but hated that everyone just ran away from me until the end of the match.
Unless they were significantly better geared and could 1-shot me.
Since then, the Battle Royale was removed from the game, and Pearl Abyss decided they'd jump into the whole BR craze and try to make Shadow Arena a standalone title. Kinda like what Ashes of Creation did with Apocalypse.
Plan 8 – I don't think we ever really knew about Plan 8 – but here we are, a brand new MMO shooter.
Pearl Abyss really are trying quite hard to expand into other niches, huh?
Plan 8 is, interestingly enough, spearheaded by the co-creator of the entire Counter-Strike franchise.. which could actually end up being really promising. "could" being the keyword here.
Not much is known other than it'll be an "exosuit MMO shooter." Make of that what you will.
Crimson Desert – I know, I know. None of you care about this one, right? It's only Pearl Abyss's next upcoming open-world fantasy-themed MMORPG from the game design director of Risk Your Life Online.
It's only going to be an even better looking, potentially PvE-themed MMO successor to Black Desert Online.
Oh, wait, I'm wrong? This is what you were actually looking for info on? Whoops. My bad. Well, then, allow me to elaborate on this one for you!
In an interview with Pearl Abyss recently, they revealed that the game engine for Black Desert was getting old and felt a little.. dated.
I don't think this is true – I feel like BDO still looks amazing but Pearl Abyss are obsessed with making games that look better and better so who am I to question them.
With this in mind, they wanted to take the time to develop new games – including MMOs on a brand new engine. This way they aren't limited by "old tech." Fast forward to 2018 when Crimson Desert began development.
Pearl Abyss wanted to make something even faster, even better looking – with combat that made Black Desert look like a thing of the past.. so they decided to bring on the lead combat designer of Risk Your Life Online and C9: Continent of the Ninth.
He'd be in charge of making certain that the combat would be possible of taking things to the next level. Honestly, C9 still has great combat – you can ask anyone that still actively plays the game what they think of it.
And Risk Your Life? People continue to talk about that game to this day.. they're both titles that have left lasting impressions on the community and I'm honestly excited to see where, specifically, Crimson Desert will go.
I know that it's possible to get action combat better than BDO, I do. I just didn't think we were at a point that required it yet.
Crimson Desert will take place on the continent of Pywell. It'll be set in the middle of a war between three different tribes, all vying for survival and dominance.
And.. that's pretty much it.
That's all that's known regarding any of the games.
DokeV looks like something really cute that you can play with your kids. But at the same time it might be something entertaining for people of all ages. We'll have to wait and see.
Shadow Arena likely won't take off – I very, very highly doubt that.
Plan 8 is an interesting concept. I can see it doing well if handled correctly, but is there room for a South Korean Counter Strike game?
And finally, Crimson Desert could be amazing. It has the potential to be something truly groundbreaking, truly epic.
If it takes a more traditional route in terms of content – adding in things that players have been asking for for years now, like Dungeons, Raids and other group-related content.. we could see something actually challenge WoW or Final Fantasy XIV.
But with the track record of Pearl Abyss.. at the same time it's highly unlikely to be nearly that good.
Then we have the problem of pay-to-win, which is an ever prevalent problem in their games. It's probably the most complained about thing in Black Desert.
But overall, with the success of Black Desert, and the current popularity of both Black Desert for the PC and console, along with the high anticipation for Black Desert Mobile.. do we really need something to replace it?
Will it even be replaced? Is that the goal of the game or are we instead going to have the game run concurrently with Black Desert?
Like take a moment and think.. one of the reasons why large companies don't normally push out new MMOs when they have an already successful-title is because they'll take attention, players and even other devs from the current game.
Do we want the playerbase to be split between Black Desert and Crimson Desert?
Do we need Crimson Desert so desperately that it'll be at the expense of Black Desert? I don't think so, and I don't believe that's what Pearl Abyss are aiming for.
But if that's not their goal, and the vast majority of Action MMORPG players already play BDO.. then what is the purpose of Crimson Desert?
Crimson Desert's main competition would be.. Black Desert. Which makes absolutely no sense.
If you play BDO then you know that it's a game that requires a lot of time and effort devoted to it. You can't just play it on and off casually.
Or, well, okay you can, but you're not going to be able to do it competitively. So if you want to play competitively, you're going to need to dedicate a lot of time to it.
And if you opt to dedicate large amounts of time to the game – like players currently do, you don't really have much time for another MMO. Which applies to all MMOs, really.
That's part of what makes an MMO an MMO, and is actually something people genuinely miss about the genre.. dedicating large amounts of their life to a game that is worth dedicating time to.
But overall, Crimson Desert's success can only come off of a reduction of active players in Black Desert.
The only way it won't, is if it's an entirely different kind of game.
Like Black Desert's current active playerbase has absolutely no effect on Final Fantasy XIV's playerbase.
BDO is an action MMO with no story, dungeons, raids or competitive PvE scene. Yet it has a highly active PvP community.
Final Fantasy XIV is an MMO with a ton of story, lots of dungeons, raids, and a lot of PvE content to do.. but at the same time doesn't have much of a PvP community.
So the two games in no way have a conflict of playerbase, nor do they impact each other's populations. Well, not unless you play both games. But the percentage of players that do is probably fairly small.
However, from what little we know of Crimson Desert.. it's going to be an Action MMORPG set in a large fantasy-themed world, with a large emphasis on PvP. So, yeah.
Similarities are shared with BDO. Far too many for it to be anything other than the successor to it..
So then that begs the question: If Crimson Desert is essentially the 2020 version of Black Desert – enhanced graphics, improved combat, more traditional features like dungeons and raids, but not at the expense of PvP and freedom.. will you guys migrate over?
Or do you think you're going to remain in Black Desert?
And, if you don't plan on moving games, what do you think Pearl Abyss are doing creating direct competition for their own game?
Do you think they're trying to capitalize on the success of BDO and are attempting to have 2 popular MMOs concurrently?
Or do you think that since launching on various consoles, PC, and now also on mobile.. they've come to the realization that from this point on, they're likely going to stagnate, and have therefore come to the realization that it's time to move on?
I'm not a game developer so I can't say, but I know Pearl Abyss are a money-hungry organization, like many are.
I understand the need and reasoning behind expanding – I do. I'm not angry nor do I harbor any ill-will towards the game when it eventually goes live.
But I'm just curious their reasoning behind it.
Should they really sacrifice everything they've built up 'til this point to build something new?
Or, maybe sacrifice is too strong of a word.
But let's be real here.. they'll be sacrificing two important things: The rate of new content produced for Black Desert, because Crimson Desert will take precedence henceforth.
And team-size, as there will likely be some shift in active team members working on the game so even though the rate of new content will be reduced, the scope of new content will also lessen.
Iunno. I'm excited for the game but like all new MMOs, especially South Korean MMOs.. Just because I'm excited doesn't mean I'm highly anticipating it.
I think it could end up really epic, but at the same time.. I feel like it could be just another flop.
Either way, on November 13th we'll get the first official trailer for the game.
Furthermore, on November 14th we'll likely receive some actual, solid information on the game.
So this is all speculation that will likely have a more concrete answer when the event is over. But it's something to think about and ponder while waiting until next week.
Maybe even get a little excited for.
The 10 Most Played MMORPGs in 2020 - What MMOs Should You be Playing? Reply
Feb 1, 2020 @ 15:42 pm
[…] are new MMORPGs to look forward to. Blue Protocol, Project TL, New World, Phantasy Star Online 2, Crimson Desert. Yet you might be wondering, until thoses new games actually release in a playable state, what MMOs […]


text:
package org.onosproject.drivers.oplink;

import org.onlab.util.GuavaCollectors;
import org.onosproject.net.OchSignal;
import org.onosproject.net.PortNumber;
import org.onosproject.net.behaviour.LambdaQuery;
import org.onosproject.net.driver.AbstractHandlerBehaviour;

import java.util.Set;
import java.util.stream.IntStream;

import static org.onlab.util.Spectrum.CENTER_FREQUENCY;
import static org.onosproject.drivers.oplink.OplinkOpticalUtility.CHANNEL_SPACING;
import static org.onosproject.drivers.oplink.OplinkOpticalUtility.STOP_CENTER_FREQ;
import static org.onosproject.drivers.oplink.OplinkOpticalUtility.START_CENTER_FREQ;

/**
 * Lambda query implementation for Oplink netconf devices in C band.
 *
 * 96 lambdas with 50GHz width (fixed grid).
 *
 * Channel id: Nominal central frequency = 193100 GHz + spacingMultiplier * channelSpacing).
 * Channel (-35 to 60): starting from 191350 GHz to 196100 GHz, Increment by 50GHz.
 */
public class OplinkOpticalLambdaQuery extends AbstractHandlerBehaviour implements LambdaQuery {

    private static final int MIN_CHANNEL = (int) Math.round(
            START_CENTER_FREQ.subtract(CENTER_FREQUENCY).asHz() / CHANNEL_SPACING.frequency().asHz());
    private static final int MAX_CHANNEL = (int) Math.round(
            STOP_CENTER_FREQ.subtract(CENTER_FREQUENCY).asHz() / CHANNEL_SPACING.frequency().asHz());

    @Override
    public Set<OchSignal> queryLambdas(PortNumber port) {
        return IntStream.rangeClosed(MIN_CHANNEL, MAX_CHANNEL)
                .mapToObj(x -> OchSignal.newDwdmSlot(CHANNEL_SPACING, x))
                .collect(GuavaCollectors.toImmutableSet());
    }
}

redpajama_set_name: RedPajamaGithub