The admission process can be complicated, but we're here to help! This page addresses the most frequently asked questions about our evaluation process.
Still have questions? Check the status of your application in Bear Tracks or Contact Us.
Most Canadian high school applications will be assessed within 1-2 weeks, assuming you have submitted enough relevant information. Other types of applications can take longer to process.
How likely am I to receive an offer?
If your marks are highly competitive, you may be admitted based on your Grade 11 marks alone, but most students need to present some final Grade 12 marks before receiving an offer. If you are not eligible the first time you are assessed, you may be asked to submit more courses and marks (and/or other required documents), at which point you may be re-assessed.
You can check the status of your application in Bear Tracks. All information related to your application and admission status will be found under the Admissions tab. Be sure to check your To-Do List, Advisor Comments, and Official Correspondences.
Any time there is an update to your admission status, you will receive an email notification directing you to check Bear Tracks. You will not receive any paper/mail correspondence from the Registrar's Office.
You are advised to include two program choices on your application. This gives you the best chance of receiving an admission offer.
When you submit two program choices on your application, you will indicate one as your top choice or priority, and one as your second choice.
You will first be evaluated for your first-choice program. If you are eligible for your first-choice program, you will receive an offer for that program, and you will not be evaluated for your second-choice program, regardless of whether you choose to accept your first offer or not.
You will be evaluated for your second-choice program only if you are not immediately eligible for your first-choice program.
If you receive an offer to your second-choice program, you are advised to accept it, even if your evaluation for your first-choice program is still pending. You will still have the option to accept an offer to your first-choice program later, should you receive one.
In many cases, you can still get admitted to your first-choice program, even if you were at first deemed ineligible, and/or you have accepted an offer to your second-choice program. Check your admission status and official correspondences in Bear Tracks to find out if and how you can be reconsidered for your first-choice program (i.e. what outstanding requirements you still need to meet).
After you apply, you can request to change your program choices or priorities on your application. You can do so by filling out the Program Change Request Form. Please take careful note of the deadlines and instructions on the form.
You will be evaluated for scholarships based on your admission average as calculated at the time of your admission offer. You will not be re-evaluated for scholarship eligibility or value a second time, even if your marks increase or decrease.


What is online chat? Online chat can refer to any kind of communication over the Internet, but is primarily meant to refer to direct one-on-one chat or text-based group chat (formally also known as synchronous conferencing), using online chat software such as instant messengers, Internet Relay Chat, chat clients and possibly MUDs. The expression "online chat" comes from the word chat which means "informal conversation". What is a chat room? People usually meet in online chat rooms to socialize. A chat room is a virtual place where people meet new friends in order to socialize for free. Visual chat rooms add graphics to the chat experience, in either 2D or [[3d-chat (employing virtual reality/gaming technology). Visual chat rooms are characterized by using a graphic representation of the user avatar that can be moved on a graphic background or within a graphic environment. These virtual worlds are capable of incorporating elements such as games (in particular massively (multiplayer online games) and educational material. The most popular environments also allow users to create or build their own spaces. Free online chat in Club Cooee When a member logs into the Club Cooee client, he or she has the option to engage in free 3D chat with other avatars. 3D chat is simply the act of talking with other members using text-based chat in a virtual world environment. Members, through the use of an avatar, have the opportunity to interact with each other and the Club Cooee 3D virtual world while expressing themselves using animations and 3D chat. In Club Cooee, members engage in shared media experiences by listening to the same music, simultaneously viewing the same information in a browser (e.g. YouTube videos, personal websites), looking at the same graphics (photos, illustrations) placed in frames on a wall in a 3D room or by playing virtual games together. 3D chat adds another dimension to the standard text-based chat experience by enhancing communication between avatars.


text:
National Eclipse
2023 Eclipse Maps
2023 Eclipse Overview
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2023 Eclipse Events
2023 Lodging & Camping
2024 Total Cities
Eclipse Animations
Eclipse Safety
Eclipse History
Eclipse Calendar
Eclipse Trivia
Eclipse Resources
National Eclipse Blog
Get Eclipse Updates
On August 12, 2045, a total solar eclipse will occur in the U.S., the Caribbean, and South America. In the U.S., the path of totality will cross over California, Nevada, Utah, Colorado, New Mexico, Oklahoma, Kansas, Texas, Arkansas, Missouri, Mississippi, Louisiana, Alabama, Florida, and Georgia. In the Caribbean, the path of totality will cross over The Bahamas, the Turks and Caicos (United Kingdom), Haiti, the Dominican Republic, and Trinidad and Tobago. In South America, the path of totality will cross over Venezuela, Guyana, Suriname, French Guiana (France), and Brazil. The maximum duration of totality for this eclipse will be 6 minutes and 6 seconds. The maps below show the path of totality over the U.S., the Caribbean, and South America. To experience the total phase of the eclipse, you must be located within the path of totality represented on the maps below. Areas outside the path of totality will get a partial solar eclipse only.
In the U.S., a partial solar eclipse will also occur in Alaska, Arizona, Connecticut, Delaware, Hawaii, Iowa, Idaho, Illinois, Indiana, Kentucky, Massachusetts, Maryland, Maine, Michigan, Minnesota, Montana, North Carolina, North Dakota, Nebraska, New Hampshire, New Jersey, New York, Ohio, Oregon, Pennsylvania, Rhode Island, South Carolina, South Dakota, Tennessee, Virginia, Vermont, Washington, Wisconsin, West Virginia, and Wyoming.
Total Solar Eclipse of August 12, 2045
Map 1 — USA
Map 2 — Caribbean and South America
UPCOMING ECLIPSES
SEE A MAP OF ALL 21ST CENTURY TOTAL SOLAR ECLIPSES IN THE CONTIGUOUS U.S.
AUSTRALIA/ASIA - HYBRID SOLAR ECLIPSE MAP - APRIL 20, 2023
USA/CENTRAL AMERICA/SOUTH AMERICA - ANNULAR SOLAR ECLIPSE MAPS - OCTOBER 14, 2023
MEXICO/USA/CANADA - TOTAL SOLAR ECLIPSE MAPS - APRIL 8, 2024
SOUTH AMERICA - ANNULAR SOLAR ECLIPSE MAP - OCTOBER 2, 2024
ANTARCTICA - ANNULAR SOLAR ECLIPSE MAP - FEBRUARY 17, 2026
RUSSIA/GREENLAND/EUROPE - TOTAL SOLAR ECLIPSE MAP - AUGUST 12, 2026
SOUTH AMERICA/AFRICA - ANNULAR SOLAR ECLIPSE MAP - FEBRUARY 6, 2027
AFRICA/EUROPE/MIDDLE EAST - TOTAL SOLAR ECLIPSE MAP - AUGUST 2, 2027
SOUTH AMERICA/EUROPE/AFRICA - ANNULAR SOLAR ECLIPSE MAP - JANUARY 26, 2028
AUSTRALIA/NEW ZEALAND - TOTAL SOLAR ECLIPSE MAP - JULY 22, 2028
AFRICA/EUROPE/MIDDLE EAST/ASIA - ANNULAR SOLAR ECLIPSE MAP - JUNE 1, 2030
AFRICA/AUSTRALIA - TOTAL SOLAR ECLIPSE MAP - NOVEMBER 25, 2030
AFRICA/ASIA - ANNULAR SOLAR ECLIPSE MAP - MAY 21, 2031
CENTRAL AMERICA - HYBRID SOLAR ECLIPSE MAP - NOVEMBER 14, 2031
SOUTHERN OCEAN - ANNULAR SOLAR ECLIPSE MAP - MAY 9, 2032
RUSSIA/USA - TOTAL SOLAR ECLIPSE MAP - MARCH 30, 2033
AFRICA/MIDDLE EAST/ASIA - TOTAL SOLAR ECLIPSE MAP - MARCH 20, 2034
SOUTH AMERICA - ANNULAR SOLAR ECLIPSE MAP - SEPTEMBER 12, 2034
NEW ZEALAND/PACIFIC - ANNULAR SOLAR ECLIPSE MAP - MARCH 9, 2035
ASIA - TOTAL SOLAR ECLIPSE MAP - SEPTEMBER 2, 2035
CARIBBEAN/AFRICA - ANNULAR SOLAR ECLIPSE MAP - JANUARY 5, 2038
SOUTH AMERICA/CARIBBEAN/AFRICA - ANNULAR SOLAR ECLIPSE MAP - JULY 2, 2038
AUSTRALIA/NEW ZEALAND - TOTAL SOLAR ECLIPSE MAP - DECEMBER 26, 2038
USA/CANADA/GREENLAND/EUROPE - ANNULAR SOLAR ECLIPSE MAP - JUNE 21, 2039
ANTARCTICA - TOTAL SOLAR ECLIPSE MAP - DECEMBER 15, 2039
AFRICA - TOTAL SOLAR ECLIPSE MAP - APRIL 30, 2041
ASIA/PACIFIC - ANNULAR SOLAR ECLIPSE MAP - OCTOBER 25, 2041
ASIA - TOTAL SOLAR ECLIPSE MAP - APRIL 20, 2042
ASIA/AUSTRALIA/NEW ZEALAND - ANNULAR SOLAR ECLIPSE MAP - OCTOBER 14, 2042
RUSSIA - TOTAL SOLAR ECLIPSE MAP - APRIL 9, 2043
SOUTHERN OCEAN - ANNULAR SOLAR ECLIPSE MAP - OCTOBER 3, 2043
SOUTHERN OCEAN - ANNULAR SOLAR ECLIPSE MAP - FEBRUARY 28, 2044
GREENLAND/CANADA/USA - TOTAL SOLAR ECLIPSE MAP - AUGUST 23, 2044
NEW ZEALAND/PACIFIC - ANNULAR SOLAR ECLIPSE MAP - FEBRUARY 16, 2045
USA/CARIBBEAN/SOUTH AMERICA - TOTAL SOLAR ECLIPSE MAP - AUGUST 12, 2045
PAST ECLIPSES
SEE A MAP OF ALL 20TH CENTURY TOTAL SOLAR ECLIPSES IN THE CONTIGUOUS U.S.
ANTARCTICA - TOTAL SOLAR ECLIPSE MAP - DECEMBER 4, 2021
CANADA/GREENLAND/RUSSIA - ANNULAR SOLAR ECLIPSE MAP - JUNE 10, 2021
SOUTH AMERICA - TOTAL SOLAR ECLIPSE MAP - DECEMBER 14, 2020
AFRICA/MIDDLE EAST/ASIA - ANNULAR SOLAR ECLIPSE MAP - JUNE 21, 2020
MIDDLE EAST/ASIA/PACIFIC - ANNULAR SOLAR ECLIPSE MAP - DECEMBER 26, 2019
SOUTH AMERICA - TOTAL SOLAR ECLIPSE MAP - JULY 2, 2019
USA - TOTAL SOLAR ECLIPSE MAPS - AUGUST 21, 2017
SOUTH AMERICA/AFRICA - ANNULAR SOLAR ECLIPSE MAP - FEBRUARY 26, 2017
AFRICA - ANNULAR SOLAR ECLIPSE MAP - SEPTEMBER 1, 2016
ASIA/PACIFIC - TOTAL SOLAR ECLIPSE MAP - MARCH 9, 2016
Featured Eclipse Offers and Destinations
CONTACT US TO PROMOTE YOUR ECLIPSE OFFER OR DESTINATION HERE
© NationalEclipse.com
Always follow safe eclipse viewing procedures!

redpajama_set_name: RedPajamaCommonCrawl


The description says "ALC contains recordings of speakers that are either intoxicated or sober." Is there a third kind of person?
I assume they're serious, becuase none of the posts are dated April 1.
The price is 1000 euros give or take plus VAT; ELRA jitters their prices, so the real price is 1020 euros plus VAT, though you might see if they'll take 1019.99.
Here's the README, including ASCII art logo.
Schiel, F., Heinrich, Chr., Barfüßer, S., Gilg, Th. (2008). ALC – Alcohol Language Corpus. In: Proc. of LREC 2008, Marrakesch, Marokko.
What's next, the Drunk American College Student Corpus from LDC?
This entry was posted on April 24, 2009 at 11:52 am and is filed under Carp's Blog.	You can follow any responses to this entry through the RSS 2.0 feed. You can leave a response, or trackback from your own site.
Would be more fun to make your own.
I bet higher BAC correlates to higher language model likelihoods: simpler language is easier to predict.
Ah, but more clearly articulated language is easier to understand bottom-up, and with HMM-type speech recognizers, it's all about the p(words|acoustics) being proportional to p(words) * p(acoustics|words). That is, a mix of the top-down predictions in the form of a language model p(words), and bottom-up predictions in the form of an acoustic model p(acoustics|words).
Perhaps the real point is that the acoustic models, even the fairly large Gaussian mixture models for p(acoustics|words), are closely fitted to their acoustic environments and population of speakers.
To make the task really challenging, they'd have done the recordings in a Biergarten.
In the forensic context it's important to know to what extent common forensic phonetic parameters differ with respect to normal un-influenced speech.


Beyond the value extension of content through repurposing is the function of personalizing content for different markets and using a modular approach to segmenting useful information for specific audience targeting.
Before you repurpose, reuse, and refresh content there are a few things to think about first.
Personas: Who is your audience?
Editorial: What topics will you use to engage with them?
Content: What materials to use to engage with them?
When identifying personas, also include who their influencers are (roles, vendors, companies). A good persona provides insight for content ideation, creation and marketing.
Editorial Topics. Talk about content that relates to what customers care about relevant to your products and services. When you have to create a large amount of content, start with broad topics.
2. It takes time, budget and effort to repurpose, reuse and repackage.
Start with flagship content and connect the dots by pulling in materials form different pieces of content.


Audience/Genre: New Adult, Urban Fantasy, Paranormal.
Publication: October 10th 2013 by Curiosity Quills Press.
plunging us into dusty darkness. Cara let out a shriek.
shriek, she dived underneath her seat to retrieve it.
could feel a headache building behind my temples.
looking down at the confusion below. Then they locked onto me.
those sinister, alien eyes, I felt exactly the same.
moment in horror stories when someone saw a ghost.
believed in them, which up until now, I thought I didn't.
bubble of horror enclosed me like the cage I'd envisioned earlier.
Then I heard a faint whisper, almost like a breath.
in the rafters, like a single patch of mist left behind after a fog has lifted.
Not a single speck of dust disturbed the area around it.
insides of my eyelids, light purple, glowing and staring.
dropping them. I didn't remember anything but those awful eyes.
Cara tried to laugh off her moment of panic.
"I didn't really think it was the end of the world," she insisted.
The end of the world. Maybe that was what I'd seen. A sign.
Visit the Darkness Watching book blitz for a list of participating blogs and to to learn more about the book.
Emma L. Adams spent her childhood creating imaginary worlds to compensate for a disappointingly average reality, so it was probably inevitable that she ended up writing fantasy and paranormal for young adults. She was born in Birmingham, UK, which she fled at the first opportunity to study English Literature at Lancaster University. In her three years at Lancaster, she hiked up mountains, skydived in Australia, and endured a traumatic episode involving a swarm of bees in the Costa Rican jungle. She also wrote various novels and short stories. These included her first publication, a rather bleak dystopian piece, and a disturbing story about a homicidal duck (which she hopes will never see the light of day).
Interesting - I like the kind of creepy eyes on the cover.


Cheap Houses For Rent In Los Angeles County - Most americans like to lease lofts instead of acquire In connection to the space some should need to search for lofts in Richmond ky that are right away automobiles In the event that you wish to lease a loft in LA, there are a few a multitude elements you need to bear in mind The Monroe condos are amongst the spots which you can right away decide on to live in.
undertaking to find a few data on the business you are considering the fact that leasing from. In case you're a advancement organization that completes a high amount of quantity you may touch base at the intersection where you have to finish that you might want to have your overwhelming tools as opposed to perpetually leasing your hardware using shoddy moving businesses in Angeles doesn't really boundaries the bore of administration which you will get.
Start by pondering why you would love to go back home, to begin with. You wanted to have interaction in your home with families and spouse's mother acquiring home requests inside and outside agreement attraction obtaining a apartment or merchandising a condo in Los Angeles is the very muddled and feverish methodology selling your present home can cause a huge upfront installment on a littler home or apartment suite. proudly owning condo houses may be stupendous speculation should you do it shrewdly. In the event that you can't buy an extravagance home car parking zone you may likewise practice the decision of leasing an extravagance condo in the city of the stars.


The stand consists of an aluminium panel complete with Perspex tubes and graduated rules for falling head permeability tests and water tank adjustable in height for constant head permeability tests. Including plastic tubing and valves.
Permeameter stand, 4 cell capacity. Wall mounting.


text:
Q: Flexible traffic & bandwidth monitor I have looked around, but have not found anything to meet our needs. I need something that can log all connections & bandwidth consumption. We need it for analysis: by protocol, source IP (& MAC if possible), destination, etc. Ideally we are looking for something that can produce custom graphs & also uses mysql. All connections go through one server on a bridged connection (2 network cards) so it is easy to pickup traffic. We are not concerned so much with internal LAN traffic as what passes in & out to the firewall. Thanks for you suggestions.
Update: I use Ubuntu 10.04

A: Previously, I posted a question about IP/host-based network traffic grapher. I am not sure if it will meet all your requirements. Have a look at this post. I tried ntop and it seems to be a very good tool.

A: Analog-X  Netstat Live is totally free.

redpajama_set_name: RedPajamaStackExchange


text:
> embeddable npm local_modules

With `local_modules` you can develop your node.js library code in your application, as if they were node_modules published on npm.

**Benefits**
- your module contains all it's dependencies
- require your local modules with absolute paths (no more: `require('../../../../server/controller.js')`)
- your application's package.json does not get bloated.
- you can publish your application that contains `local_modules`
- the `local_modules` dependencies get installed
- your `local_modules` do not have to be developed inside the `node_modules` directory.
- it supports your development workflow and installs `local_modules` as local npm modules.

**why would I need a module for this?**

> read: [MOTIVATION](MOTIVATION.md)

**whow does it work?**

- during *development*, it installs your local modules dependencies and links and links your local modules into the `node_modules` directory.

  Run:

  ```
  lm link -f
  ```

- when installing your app in *production*, it temporarely adds `file:` dependencies to your `package.json` and runs `npm install` to install your local modules and their dependencies. Afterwards it restores your original `package.json` file.

  Run:

  ```
  lm install -f
  ```

# install

```sh
npm i -g local_modules
```

# use

> you can use `local_modules` from the code in node.js or via command line.

If you wan't to publish your module that contains `local_modules` to npm, you can add this script to your `package.json`.

**preparation**

```js

  "scripts": {
    "postinstall": "local_modules install -f",
    ...
   }

```

**development**

to **link** the local modules of your app into node_modules **and install their dependencies**, run:
```sh
lm link -f
```

**production/deployment**

to **install** the local modules of your app, run:
```sh
lm install -f
```

### command line

> `lm` is the alias for `local_modules`. you can use either one.

```sh
lm -h

*lm* helps you to deal with local npm modules.
It installs local modules and it's dependencies, e.g. useful in production,
and links them to have always up to date modules e.g. during development.

Usage: lm <command> [options]

lm -h      show help
lm -v      print lm version

Commands:

install    temporary adds the local module to the package.json, runs `npm install`, and removes them from package.json again.
uninstall  removes the local modules from the package.json, and runs `npm prune`, to remove the unneeded but installed modules.
link       links the local modules into the `node_modules` folder.
unlink     removes links of the local modules inside the `node_modules` folder.
add        adds the local modules to the package.json
remove     removes the local modules from the package.json

Options:
--dir      local module dirname default:`local_modules`
--tmp      temporary package.json file ending during install
--force    forced action: remove stuff, before copying or linking

```

```sh
# example
// install local modules in `./lib` directory
lm install --dir lib

```

### code

```js

// install example
var lm = require('local_modules');
lm({cmd: 'install', dir: 'lib'});

// or link example
lm({cmd: 'link', dir: 'lib', force: true});

```

# test

```sh
npm test
```

# license
MIT

# author
Andi Neck [@andineck](https://twitter.com/andineck)

redpajama_set_name: RedPajamaGithub


I have no medical, nutrition, pharmaceutical, or cooking background!!
However, I did run out of my flax seed pills once, so I had to get creative. I had grinded flax seeds at home in a bag. They taste really bad mixed with pretty much with anything, so I boiled them and then filtered that. I drank the juice that came out. Here are some pictures of my EvIl InVeNtIoN.


I'm innocent! I swear it! I didn't set out to be a mystery writer. I'm a victim of circumstances!
My sabbatical projects: 1) learn a bunch of violin concertos that had gathered dust on my music stand; 2) compose a string quartet; 3) write a violin method book, covering universally encountered problems students have: playing in tune, performance anxiety, preparing for auditions, buying a violin. Every chapter would be a violin lesson.
Fast forward twelve years and twice as many rewrites. Violin Lessons has morphed into Devil's Trill. Most of the technical violin stuff has mysteriously vanished, though we do delve into so many dark corners of the classical music world that concertgoers are now accompanied by personal bodyguards. Daniel Jacobus has become so irritatingly popular (crusty on the outside but deep down he has a heart of gold…maybe) that he's also the protagonist of Danse Macabre, Death and the Maiden, and Death and Transfiguration, all published by St. Martin's Press. All four titles are pieces of music that have to do with death. It has oft been said that music soothes the savage breast. One could also say, music kills. But I didn't. I'm innocent, I tell you.
Gerald Elias brings over thirty-five years as an internationally acclaimed concert violinist, conductor, composer, and teacher to his novels that take place in the murky recesses of the classical music world. He has been a violinist with the Boston Symphony and associate concertmaster of the Utah Symphony, and has concertized on five continents. He draws upon his intimate familiarity with the unseen drama behind the curtain to shed an eerie light on the deceptively staid world of the concert stage.
In addition to being an essayist and writer of short stories, Elias is author of the award-winning Daniel Jacobus mystery series (St. Martin's Press). His first novel, Devil's Trill, was selected by Barnes and Noble for its Discover: Great New Writers 2009 catalog. His second, Danse Macabre, was named one of the top five mysteries of 2010 by Library Journal and Book of the Year in fiction by the Utah Humanities Council. The third installment of the series, Death and the Maiden, was released in 2011, and his latest novel, Death and Transfiguration, received three starred reviews.
A native New Yorker, Elias now resides in Salt Lake City, Utah, and West Stockbridge, Massachusetts. He remains active as a concert artist, and continues to expand both his musical and literary horizons.
Learn more at www.geraldelias.com or https://www.facebook.com/gerald.elias.
Don't forget - Chapter 1 of Death and Transfiguration right here on Wednesday!


text:
Xbox Addict Asylum > Original Xbox > General Discussions > Kakuto Chojin - my review
View Full Version : Kakuto Chojin - my review
skysaw
Was looking forward to this title for six months. Bought it yesterday, and played it with my girlfriend for a couple of hours last night. Returned it today. Here's why.
1. We hated the characters. There's only two or three that have any visual appeal at all to me. I like the idea of a dark feeling to the graphics, but I just didn't like the character design. Why do they all need to look like super-villians taken from an old Batman comic?
2. The scenes have no variety. They are all fairly small arenas, and have generally the same look to them. There were no differences in play, either (compare to DOA3 where strategy changes per scene).
3. VS mode not well thought-out. After every match, you have to reselect a character, costume, fighting style, and location -- you can't just say "play again." It also does not keep track of wins/losses. We kept just choosing the first arena since it was half a second quicker, and they all looked about the same. There is no location randomizer.
4. Very limited number of accessible moves, and few were very interesting. I don't feel like I need spectacular flying through the air on fire, twirling, magic attacks, but I wouldn't mind seeing a few more interesting moves now and then. We were never able to perform more than one throw per character, and there were no counter-attacks, except for a throw counter which just looked like a regular attack.
5. I played through story mode with one character to unlock the "Chojin" fighting style. I could not tell the difference between the two styles.
I feel pretty dissappointed. I was really excited to finally play this game, but it just didn't deliver. Yes, the graphics are very good, but they are in no way appealing in a "gee, this is fun to play/watch" sense. The only thing I really liked about them was the reflections on the floor -- quite nice in fact. The colored lighting was cool, but it seemed a bit arbitrary. It was there to some degree in every arena, and seemed to shift around for no reason.
I do intend to try out all the upcoming fighters. But so far, nothing is touching DOA3. I'm guessing my girlfriend and I have beaten each other to a pulp several thousand times, and we're still not bored of it. We're still discovering new strategies, and laughing our asses off at the little surprises that sometimes come up in game.
RudedogX
Good review. Thanks for the heads up!:)
You just confirmed all of the reviews from the other sites, and since you're on this site, I'm definetly more apt to believe someone who's not paid to be a critic.
mmattai
I could have told you KC would suck :) I've seen videos of the gameplay and it just looked so bad. Character models would look sweet and tempt me to check it out, then I would see it in action and remember why I hated it. My friends and I still have DOA3 tournaments for hours. I don't expect a good fighter until Soul Calibur 2 comes out. Mortal Kombat: Deadly Alliance looks horrible. Jury is still out on Tao Feng: Fist of the Lotus until I see more videos. And I'm still waiting for confirmation news about Virtua Fighter 4.
I had heard it would suck, but wanted to try it to make sure. I've disagreed with the masses on more than one occasion, after all. Anyway, I guess I was in denial, since I really wanted it to be good.
I'm going to give MK and Tao Feng both a chance too, since I can always return 'em. I don't necessarily need any of them to be better than DOA3, but in the same ballpark would keep it in my collection.
Another year till DOA4. *sigh*


text:
Q: Divide all columns by another column. Also divide all columns by aggregate function(min, max, sum, count, etc.) I'm guessing this is not possible without defining a function. The idea is that you have a table like
table:
----------------
| A | B | Total|
|---|---|------|
| 1 | 2 |  3   |
| 4 | 5 |  9   |
| 6 | 7 | 13   |
----------------

select */Total from table

----------------------------
|   A   |   B   |   Total  |
|-------|-------|----------|
| 0.333 | 0.667 |  1.00    |
| 0.8   | 0.556 |  1.00    |
| 0.462 | 0.538 |  1.00    |
----------------------------

select */(select max(*) from table) from table

----------------------------
|   A   |   B   |   Total  |
|-------|-------|----------|
| 0.167 | 0.286 |  0.231   |
| 0.667 | 0.714 |  0.692   |
| 1.000 | 1.000 |  1.000   |
----------------------------

A: So you want operators on your output. You can simply do this to get your first example:
SELECT A/total, B/total, (A+B)/total FROM `table`

You don't even need a 'total' column:
SELECT A/(A+B), B/(A+B), 1 as total FROM `table`

Second one, if you are trying to get the average, same logic applies.


Westmeath Volunteer Centre, as part of their commitment to support and promote volunteering have recently introduced a new Garda Vetting service for voluntary and community groups within their local areas. We can now act as an Authorised Signatory for Garda Vetting purposes for voluntary and community organisations which do not have access to an authorised signatory within their own parent organisation.
There is an administration fee of €10 charged by Westmeath Volunteer Centre for the processing of Garda Vetting Forms for Volunteers, a fee of €10 charged for the processing of Garda Vetting Forms for trainees and a fee of €25 charged for the processing of Garda Vetting Forms for employees/staff.
Garda Vetting is the process by which a form is submitted to An Garda Siochana Vetting Office asking them to check if a person has any convictions and/or prosecutions, successful or not, pending or completed, recorded against their name.
At present, there is no legal requirement to vet volunteers, although this may be introduced at some point. Many organisations choose to make it a policy to vet volunteers who work with children and vulnerable adults and/or are responsible for finances. However, most organisations recognise that not all volunteers may need to be vetted. For example, volunteers working in administration, doing practical work, providing professional services or a range of other volunteer opportunities may not need to be vetted as they are not interacting with the clients or directly involved in finance and will never have an opportunity to do so.
It is up to the organisation to decide whether or not a volunteer position requires vetting. This should be assessed while the organisation is in the process of developing the job description for each individual volunteer position. Whether the volunteer is being vetted or not it is important to conduct reference checks as these provide vital character reference information that is not available in a Garda vetting check. (Your local volunteer centre will supply you with in-depth information and training on the process).
Will An Garda Siochana vet our volunteers?
If your organisation does not have access to an Authorised Signatory and you require Garda Vetting, your local volunteer centre can process the vetting paperwork for your volunteers. This paperwork is then forwarded to the Garda Central Vetting Unit. A list of local centres can be found on the Volunteer Centres Ireland website at www.volunteer.ie.
Your organisation will be required to register with your local volunteer centre.
Your organisation will be required to meet with/attend training about the Garda Vetting process with your local volunteer centre.
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There are stories that make you think long after they have been read. This collection of stories are just that. Each one of them had the power to make me ponder.
The best part about this anthology was the way plots differed in each story. In fact, each one revolved around a sub-theme of the main theme. Yes, the main theme revolved around depicting negative emotions. It encompassed fear, anger, hatred, sorrow, pain, hurt, distrust; name it and it was there.
The writing actually left the readers wanting more. Jeremy's narration definitely kept the reader guessing for more. The best part about his writing style was use of words that helped bring out the essence of each story. The stories were not complete in themselves, as in, they left many questions unanswered, and thats where the beauty of this anthology lies. Every story created an imagery of a different kind. Some created vibrant visual imageries, while others created aural and tactual ones. On the whole, an excellent writing style.
Every story had differwnt set of characters. And in not one story did I feel there was an excessive usage or presence of underplayed characters. Every character succeeded in depicting an emotion vital to that particular story and helped in its smooth flow.
To sum up, the stories are amazing individually as well as a part of this anthology. It is a must read because of the writing techniques used for keeping the interest of the reader alive. For me, the USP was the way each story made me think about it long after I had finished reading.
P.S - Thanks a ton Jeremy for stories I am never going to forget. In fact I have so many questions about each one that I would be reading it again. My review is an honest opinion after I read the stories.


text:
void ptwq_set_current_thread_priority(int priority)
{
    return;
}


text:
Has not yet joined TPNW
Chad has not yet signed or ratified the Treaty on the Prohibition of Nuclear Weapons.
Chad has promoted universal adherence to the treaty, including by voting in favour of an annual UN General Assembly resolution since 2018 that calls upon all states to sign, ratify, or accede to the treaty "at the earliest possible date".
In July 2020, the Chadian foreign ministry indicated that Chad will adhere to the treaty "when the time comes".
Chad participated in the negotiation of the treaty at the United Nations in New York in 2017 and was among 122 states that voted in favour of its adoption.
In 2016, Chad voted in favour of the UN General Assembly resolution that established the formal mandate for states to commence negotiations on "a legally binding instrument to prohibit nuclear weapons, leading towards their total elimination".
Chad was among 127 states that endorsed a "humanitarian pledge" in 2015–16 to cooperate "in efforts to stigmatise, prohibit, and eliminate nuclear weapons". The pledge was instrumental in building momentum and support for convening the negotiations.


text:
Burning questions for IU football coming out of the 2020 season
January 4, 2021 by Hoosier Sports Report Leave a Comment
One memorable season is in the books.
Now the question is "What's next?"
For Indiana football, the hope is that a combined 14-7 record over the last two seasons indicates an upward trajectory. But there are significant questions as to what comes next in 2021, and those will begin to be answered in the coming days and weeks.
Here are a few burning questions for the Hoosiers heading into an important offseason.
Who is coming back?
Every year seniors leave and freshmen arrive, as is the natural order of things in college athletics.
But this year isn't normal.
Because of the pandemic and the shortened seasons that came with it, the NCAA has offered all fall athletes — as it did with spring and winter athletes — an extra year of eligibility. So players who would ordinarily have seen their eligibility run out can come back for the 2021 season.
"Some will, some won't," IU coach Tom Allen said after the Outback Bowl. "We'll know for sure here in the next couple of weeks. Either way, we're going to love and support them, whatever they feel is best for them and their future. We'll talk that through with them."
The senior class is a small but important group for IU. At the top of the list are two receivers, Ty Fryfogle and Whop Philyor. Both have done enough to at least put themselves on the radar for NFL squads as potential late-round picks. It's debatable whether an additional year would benefit their pro stock.
Fryfogle, who has developed into an intriguing possession-type receiver, was somewhat under the radar until a breakout campaign in 2020. He was the Big Ten's receiver of the year, posting the conference's first-ever back-to-back 200-yard receiving games. Can he further solidify his NFL standing with another year of catching jump balls from Michael Penix Jr.?
Philyor became the 10th player in IU history to reach 2,000-plus career yards, but the Hoosiers do have a graduate transfer arriving, Florida State's DJ Matthews, who also offers some speed and elusiveness in the slot. Would they want to share that role in 2021?
IU's offensive line would be especially veteran if center Harry Crider or guard Mackenzie Nworah decided to return. Crider, who was invited to the East-West Shrine Bowl's virtual events, has a chance to see if he could stick on an NFL roster, but coming back would give him another year as the anchor of the Hoosiers' offensive line. At the same time, IU has added a Michigan transfer, Zach Carpenter, who can play both guard and center, just like redshirt junior Dylan Powell and redshirt freshman Mike Katic.
While the defense is dominated by juniors and sophomores, it could gain from senior returnees. Jerome Johnson, a first-team All-Big Ten defensive tackle, and Marcelino Ball, an athletic "husky" who had his 2020 taken away by an ACL tear, are both fifth-year seniors. Would they want to stay a sixth year?
At least a couple of players, defensive tackle Jovan Swann and defensive end Mike Ziemba, have alluded to an interest in playing on. Ziemba, a fourth-year senior, posted a video to Twitter on Sunday saying "there's more to be done" and "it's time to get back to work." Swann, a graduate student, wasn't overly specific, either, but he posted "I'm not giving up on the game, not in that fashion. I have more to give and more to gain."
In the coming days, these players will sit down with Allen and plot a course. Any that return will only strengthen an already mature roster.
How will Penix progress?
While the focus Saturday was on the field and with Penix's backup, Jack Tuttle, there was good news regarding IU's sidelined QB coming out of the Outback Bowl.
Penix's parents, Takisha and Michael Sr., gave an interview with an ABC affiliate, and the clip featured B-roll of their son walking on IU's sideline during the game. He's only a couple of weeks removed from a mid-December ACL surgery, so he appears to be recovering well.
"When he gets back, he'll show everybody what he's made of," Michael Sr. told the ABC station. Takisha added her son should be back for the start of fall camp, echoing what Allen has already said. Michael Penix Jr. is not expected to participate in spring ball in any significant way.
Penix has been through this before. He tore the same ACL his true freshman season, and he suffered a season-ending sternoclavicular joint injury as a redshirt freshman. He gained around 15 pounds this last offseason, hoping an increase in mass would lead to better durability.
Now it's time to attack another rehab, hoping the injury bug is finally behind him. If Penix can successfully move past those worries, IU's offense becomes all the more explosive, because the lefty just has an uncanny knack for making passes not a lot of quarterbacks can make.
The question is just how much progress Penix can make physically, and if he can be 100 percent by IU's opener on Sept. 4 at Iowa.
If there are any setbacks, the Hoosiers do at least have a backup with starting experience in Tuttle. Dexter Williams, a true freshman this season, should have a more typical offseason under his belt going into 2021, and the quarterback room will add depth with four-star Donaven McCulley entering the picture.
But there isn't a doubt, IU has been at its best with Penix under center. IU is 11-1 over the last two seasons when Penix is the starter at quarterback. He was named second-team All-Big Ten in 2020, even with his season cut short.
All of Hoosier Nation collectively crosses its fingers.
Who will be the DC?
Once again, the Hoosiers head into an offseason with intrigue at a coordinator spot.
Last year, it was the offensive coordinator position, as former tight ends and quarterbacks coach Nick Sheridan replaced now-Fresno State head coach Kalen DeBoer. Now it's defensive coordinator Kane Wommack who is moving on to be South Alabama's head man.
It's positive that Allen's program can serve as a springboard for his assistants, which should only make it a more attractive destination when searching for new hires. At the same time, it again raises questions about how the Hoosiers will sustain another switch.
After one year — especially a year like 2020 — it's hard to broadly assess Sheridan's performance. Even Sheridan would admit, from time to time, he needed to do a better job of more consistently putting the Hoosiers in a position to succeed. Going from an experienced play-caller like DeBoer to a first-timer, there was bound to be at least some drop-off. But it wasn't a devastating reduction.
IU's point-per-game average went from 31.8 under DeBoer to 28.9 under Sheridan, and the latter didn't have the benefit of a non-conference season.
Can the next person at DC also hold the line? Wommack shepherded his "Swarm D" from young and inconsistent in 2019 to mature and smothering in 2020. The next leader of that unit will have a wealth of returners to work with, including All-Americans Micah McFadden (linebacker) and Tiawan Mullen (cornerback).
There is bound to be continuity between this year's defense and next year's, regardless, whether Allen pegs an internal or external candidate, because this is Allen's 4-2-5 scheme. That's not changing. It's just a question of play-calling and game-planning, and what that next person's brainpower can add.
At the very least, IU doesn't want to take a step back after leading the nation with 17 interceptions in seven games, as well as a Big Ten-best 25 sacks in eight games.
Filed Under: Indiana


Miller v. Pfizer Inc. (Roering Division), 196 F. Supp. 2d 1095, 1125 (D. Kan. ...... by the Church of Scientology, petitioned the FDA to withdraw its approval of Prozac. ..... patients' associated with the treatment of fluoxetine (Beasley et al., 1991).
Mar 1, 2018 ... Pfizer Inc. (the "Company") by Trinity Health et al. ..... Jersey, UAW Retiree Medical Benefits Trust, United Church Funds and the Ursuline ..... V. The Proposal May be Excluded Pursuant to Rule 14a-8(i)(10) Because Pfizer.
Wright Medical Group et al., No. ... Henry Schein, Inc. et al. v. Archer and ... Statutory Employee Doctrine. Rublee v. Pfizer, No. 94732-5 (Wash. March 30, 2018).
Oct 13, 2014 ... children alleged that the Pfizer company had direct liability for the company's ... ( S.D.N.Y. 2006) judgment entered sub nom.; Presbyterian Church of Sudan v. ..... 03-339, 2004 WL 425376); see also Doe I, et al., Plaintiffs, v.
Client Case Results From The Driscoll Firm P.C.
Pfizer, Inc., et al. (Case No. 2007-L-325) and in Wiese, et al. v. Pfizer, Inc., et al. ( Case No. 007-L-324) in claims involving Celebrex (confidential settlement).


text:
Opera Is Still Getting Acquired By A Bunch Of Chinese Companies – Just Not Its Lucrative Ads Biz
by Allison Schiff // Monday, July 18th, 2016 – 3:30 pm
Deals fall through all the time. But the failed acquisition of Opera's ad business could be a signal that China's western buying spree is liable to hit a few regulatory snags.
In February, a consortium of Chinese companies, which comprises mobile game maker Kunlun and security software provider Qihoo, announced its intention to buy up all of Opera's assets in a $1.2 billion bid to shore up their businesses at home and expand internationally.
"Globalization is a huge focus for many of the major Chinese companies which are looking to grow their user base abroad after they reach market dominance at home," ironSource CMO Omer Kaplan said to AdExchanger at the time.
Opera shareholders were cool with it. But regulators had another idea, and the deal failed to get the blessing of the Committee on Foreign Investment in the United States by Friday's deadline. Opera shares took a tumble.
By Monday, a restructured offer was on the table – $600 million for Opera's mobile and desktop browser business, its performance and privacy apps, its tech licensing business (excluding Opera TV) and its nearly 30% stake in nHorizon, a mobile browser company in Beijing.
The assets being sold to the China contingent will be reorganized into a separate company structure – basically all of the consumer-facing stuff plus a few bits and bobs, but none of the advertising business, including Opera apps and games, Opera's OTT arm Opera TV and Opera Mediaworks. (In a blog post, Mediaworks CEO Will Kassoy said his part of the company will continue with its growth plans and that the leadership will remain intact.)
Opera referred to the three units now no longer being included in the China deal as the "remaining businesses."
But they're quite lucrative. And the rejiggered offer is a bit odd, considering that what remains composes a large portion of Opera's business. Total revenue for the company was $163.5 million in Q1 2015. Mobile advertising was responsible for $117.1 million of that.
What went wrong? The answer may boil down to international privacy worries. Opera's China-based buyers would've been privy to mobile audience data available through its ad business.
A Kulun spokesperson told Reuters that Opera's ad unit involved "very many users' privacy," which would mean an "extremely rigorous" investigation that could have delayed the original deal by six months or a year.
The concern could stem from US regulators not wanting to create a situation in which the Chinese government has access to US users' data. Chinese tech companies can be required to turn over data if government departments ask for it.
And that could be a kink for Chinese companies getting hot on foreign M&A, of which there's been quite a lot recently.
Chinese mobile ad platform Mobvista bought app monetization company NativeX in February, and mobile SSP Smaato got scooped up by a Beijing-based offline marketing service provider called Spearhead Integrated Marketing Communications Group in June. In July, Mobvista struck again with the acquisition of Danish behavioral analytics platform GameAnalytics in July. And back in March 2015, Chinese app developer Cheetah Mobile shelled out for French mobile ad tech company MobPartner.
Why Zynga Is Buying A Hypercasual Gaming Studio Despite IDFA Restrictions On The Horizon
3 Ways Apple Is Throwing Its Weight Around The Ad Industry
Facebook's IDFA Plan: Possible Audience Network Shutdown For IOS 14
Google's Quiet Preparations For Apple's IDFA Change Offers Hints On The Future Of Its Own Mobile Ad ID


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More links for "Samos Strix 1080 Ti Graphics Card Water Block - Nickel + Plexi"


text:
\section{Introduction}
\label{sec:introduction}

Since the publication of the first preliminary orbits in the 1930's by
\cite{Christie:34, Christie:36}, the bright giant star HR~6046\
(HD~145849, HIP~79358, $\alpha = 16^{\rm h} 11^{\rm m} 48\fs05$,
$\delta = +36\arcdeg 25\arcmin 30\farcs3$, J2000.0; spectral type
\ion{K3}{2}, $V = 5.63$) has been known as a highly eccentric
$\sim$6-yr period single-lined spectroscopic binary of particular
interest. The relatively large minimum mass inferred early on for the
companion ($> 3$~M$_{\sun}$), along with the fact that it was not
visible to early observers, led to the speculation that the secondary
was a collapsed star \citep{Trimble:69}, more commonly referred to
nowadays as a black hole.  Very recently \cite{Scarfe:07} have
dispelled this notion by detecting the secondary spectroscopically and
showing that it is merely an evolved late-type star, with nothing
particularly out of the ordinary in its properties other than the fact
that it is faint. On the basis of extensive radial velocity
measurements carried out over more than 26 years these authors
presented an accurate double-lined orbit for the system yielding
minimum masses considerably smaller than previously thought. They also
found the components to be nearly identical in mass to within about
1\%, even though they are substantially different in brightness
($\Delta V \approx 3$). They relied on the {\it Hipparcos\/}\ parallax of the
system \citep{Perryman:97} to construct a plausible photometric model
of the stars (individual magnitudes and colors), but cautioned that
the distance could be vitiated by unmodeled photocentric motion.

As described by \cite{Scarfe:07}, HR~6046\ has never been spatially
resolved despite repeated attempts over the years using speckle
interferometry and other techniques. However, \cite{Jancart:05} were
able to obtain an estimate of the inclination angle by reconsidering
the {\it Hipparcos\/}\ Intermediate Astrometric Data in conjunction with the
spectroscopic orbit of \cite{Christie:36} to account for the binary
motion. With this the absolute masses of the components can in
principle be obtained, although the resulting values are somewhat high
for late-type giants ($\sim$3.6 M$_{\sun}$) possibly because of the
use of outdated spectroscopic elements.

The main motivation for the present work is to revisit the {\it Hipparcos\/}\
astrometric solution in the light of the accurate orbit of
\cite{Scarfe:07}, and to examine the effect on the published
parallax. Additionally, we investigate the evolutionary status of the
system with our newly determined masses, aided by current stellar
evolution models. We report also a spectroscopic determination of the
effective temperature of the primary star that supports the general
picture outlined by other constraints in showing the evolved state of
the binary.

\section{HIPPARCOS observations and revised astrometric solution}
\label{sec:orbit}

Given the 6-yr orbital period of HR~6046, which is of the same order as
the duration of the {\it Hipparcos\/}\ mission (slightly more than 3 yr), it may be
expected that the orbital motion would be detectable in the satellite
measurements, and that if not properly accounted for, it could bias
either the trigonometric parallax, the proper motions, or both.
Indeed, proof that a signal of this nature is detectable is given by
the fact that the {\it Hipparcos\/}\ team found it necessary to include
acceleration terms in the astrometric solution, representing the first
derivatives of the proper motions. These terms, $d\mu_{\alpha}^*/dt =
-9.08 \pm 1.23$ mas~yr$^{-2}$ and $d\mu_{\delta}/dt = -6.98 \pm 1.53$
mas~yr$^{-2}$, are statistically significant. It is unclear why a full
orbital model was not applied originally to this system, since the
binary nature of the object has been known for a long time. In any
case, this has been done more recently by \cite{Jancart:05}, as
mentioned earlier.

A total of 78 astrometric measurements were made by {\it Hipparcos\/}\ from 1989
December to 1993 February, covering about 53\% of an orbital cycle.
Each measurement consisted of a one-dimensional position (`abscissa',
$v$) along a great circle representing the scanning direction of the
satellite, tied to an absolute frame of reference known as the
International Celestial Reference System (ICRS). The measurements
available for our analysis are published in the form of `abscissa
residuals' ($\Delta v$; see Table~\ref{tab:abscissae}), which are the
residuals from the standard five-parameter solution reported in the
Catalogue \citep{Perryman:97}.  The five standard parameters are the
position ($\alpha_0^*$, $\delta_0$) and proper motion components
($\mu_{\alpha}^*$, $\mu_{\delta}$) of the barycenter at the reference
epoch 1991.25\footnote{Following the practice in the {\it Hipparcos\/}\ Catalogue
we define $\alpha^* \equiv \alpha \cos\delta$ and $\mu_{\alpha}^*
\equiv \mu_{\alpha} \cos\delta$.}, and the trigonometric parallax,
$\pi_{\rm t}$. The nominal errors of these measurements have a median
value of 2.5 mas.

We incorporated orbital motion into a new astrometric solution
following the formalism of \cite{vanLeeuwen:98}, \cite{Pourbaix:00},
and \cite{Jancart:05}, including the correlations between measurements
from the two independent data reduction consortia that processed the
original {\it Hipparcos\/}\ observations \citep[NDAC and FAST;][]{Perryman:97}.
Details of this modeling along with another example of an application
may also be seen in \cite{Torres:07b}. In the most general case the
adjustable quantities of the fit (a total of 12) are the corrections
to the five standard {\it Hipparcos\/}\ parameters ($\Delta\alpha^*$,
$\Delta\delta$, $\Delta\mu_{\alpha}^*$, $\Delta\mu_{\delta}$, and
$\Delta\pi_{\rm t}$), and the seven usual elements of the binary
orbit: the period $P$, the semimajor axis of the photocenter $a_{\rm
phot}$, the eccentricity $e$, the inclination angle $i$, the longitude
of periastron for the primary $\omega_{\rm A}$, the position angle of
the ascending node $\Omega$ (equinox J2000.0), and the time of
periastron passage $T$. For HR~6046\ the {\it Hipparcos\/}\ measurements do not
constrain $P$, $e$, $\omega_{\rm A}$, or $T$ sufficiently well, so
those elements were held fixed at their spectroscopic values as
reported by \cite{Scarfe:07}. We solved for the remaining 8 parameters
simultaneously using standard non-linear least-squares techniques
\citep[][p.\ 650]{Press:92}. The reduced $\chi^2$ of the solution is
0.9895, indicating that the internal errors of the abscissa residuals
are realistic.

We list the results in Table~\ref{tab:elements}, where they are
compared with those obtained by \cite{Jancart:05}. Significant
differences are seen in the semimajor axis and inclination angle,
which reflect the spectroscopic constraints used in each case.
Jancart's value of $a_{\rm phot}$ is nearly twice as large as ours,
and while their inclination angle is substantially smaller than
90\arcdeg, we obtain an orientation that is essentially edge-on. The
smaller $i$ value of \cite{Jancart:05} would lead to much larger
absolute masses for the stars when combined with the minimum masses of
\cite{Scarfe:07}, as noted in \S\ref{sec:introduction}.  There is
little doubt that the recent orbital elements by \cite{Scarfe:07}
supersede the provisional values of \cite{Christie:36} adopted by
Jancart, which suggests our solution should be closer to the
truth.\footnote{A preliminary version of the \cite{Scarfe:07} work had
been published in 2004 \citep{Scarfe:04}, but was perhaps not yet
available to Jancart and collaborators.} An external check on our
results is provided by the absolute proper motions we obtain, listed
in the bottom section of Table~\ref{tab:elements}. These are different
from the values reported in the {\it Hipparcos\/}\ Catalogue, which are likely to
be affected also by the unmodeled orbital motion. They agree well,
however, with the motions given in the Tycho-2 Catalogue
\citep{Hog:00}, as shown in Table~\ref{tab:pm}. The latter are based
on the position from the Tycho experiment aboard the {\it Hipparcos\/}\ satellite
(epoch $\sim$1991.25) combined with ground base catalog positions
going back nearly a century in some cases.  This long baseline tends
to average out any orbital motion that has a period of a few years, as
in the case of HR~6046, and therefore yields a more accurate estimate than
{\it Hipparcos\/}.  Finally, we note that our revised {\it Hipparcos\/}\ solution
did not change the value of the parallax significantly, which was one
of the concerns of \cite{Scarfe:07}. This parallax corresponds to a
distance of 178 pc.

\begin{figure}
\vskip -0.3in
\epsscale{1.3}
{\hskip -0.2in \plotone{f1.eps}}
\vskip -0.3in
\figcaption[]{(a) Abscissa residuals of HR~6046\ from the {\it Hipparcos\/}\ mission as
a function of orbital phase. These are the residuals from the standard
5-parameter solution as published in the Catalogue
\citep{Perryman:97}.  The systematic patterns are due to the unmodeled
motion of the center of light. (b) $O\!-\!C$ residuals of the {\it Hipparcos\/}\
measurements from our new 12-parameter fit that accounts for the
orbital motion.\label{fig:hipresid}}
\end{figure}

As a way of visualizing the effect of accounting for the orbital
motion in the {\it Hipparcos\/}\ solution, we show in Figure~\ref{fig:hipresid}a
the abscissa residuals $\Delta v$ resulting from the standard
5-parameter solution as a function of orbital phase. Some systematic
patterns are apparent, but they largely disappear after the orbital
motion is incorporated into the model. This is shown by the $O\!-\!C$
residuals from the 12-parameter fit in Figure~\ref{fig:hipresid}b.

\begin{figure}
\vskip -0.6in
\epsscale{1.3}
{\hskip -0.2in \plotone{f2.eps}}
\figcaption[]{Motion of the photocenter of HR~6046\ relative to the center
of mass of the binary (indicated by the plus sign) as seen by
{\it Hipparcos\/}. The one-dimensional abscissa residuals are shown schematically
with a filled circle at the predicted location, dotted lines
representing the scanning direction of the satellite, and short
perpendicular line segments indicating the undetermined location of
the measurement on that line (see text). The length of the dotted
lines represents the magnitude of the $O\!-\!C$ residual from the
computed location.  Three measurements with residuals larger than 5
mas were omitted for clarity. Also indicated on the plot is the
location of periastron (open circle near the
top).\label{fig:hiporbit}}
\end{figure}

The projection of the photocentric orbit on the plane of the sky along
with a schematic representation the {\it Hipparcos\/}\ measurements is seen in
Figure~\ref{fig:hiporbit}, where the axes are parallel to the right
ascension and declination directions.  Because these measurements are
one-dimensional in nature, their exact location on the plane of the
sky cannot be shown graphically. The filled circles represent the
predicted location on the computed orbit (see also
Figure~\ref{fig:deproject}).  The dotted lines connected to each
filled circle indicate the scanning direction of the {\it Hipparcos\/}\ satellite
for each measurement, and show which side of the orbit the residual is
on. The length of each dotted line represents the magnitude of the
$O\!-\!C$ residual.\footnote{The ``$O\!-\!C$ residuals'' are not to be
confused with the ``abscissa residuals'' $\Delta v$, which we refer to
loosely here as {\it Hipparcos\/}\ ``observations'' or ``measurements''. As
indicated earlier, the abscissa residuals are in fact residuals from
the standard 5-parameter fit reported in the {\it Hipparcos\/}\ Catalogue, whereas
the $O\!-\!C$ residuals (or simply ``residuals'') are the difference
between the abscissa residuals and the computed position of the star
from a model that incorporates orbital elements.}  The short line
segments at the end of and perpendicular to the dotted lines indicate
the direction along which the actual observation lies, although the
precise location is undetermined. Occasionally more than one
measurement was taken along the same scanning direction, in which case
two or more short line segments appear on the same dotted lines. The
orbit is formally clockwise (retrograde), although the orientation is
so close to edge-on ($i = 91\fdg4 \pm 9\fdg7$) that the motion on the
plane of the sky may well be direct.

\begin{figure}
\vskip -0.6in
\epsscale{1.3}
{\hskip -0.2in \plotone{f3.eps}}
\figcaption[]{Same as Figure~\ref{fig:hiporbit}, except that the orbit
has been de-projected to appear as if it were viewed exactly face-on.
The line of nodes is indicated with the dashed line. Motion on the
plane of the sky in this figure is direct (counterclockwise).
\label{fig:deproject}}
\end{figure}

The phase coverage of the {\it Hipparcos\/}\ observations is seen more clearly in
Figure~\ref{fig:deproject}, in which we have de-projected the orbit
and represented it as if it were viewed with an inclination angle of
0\arcdeg. The measurements happen to cover the periastron passage of
1991.83 (indicated with an open circle), but not apastron.  The path
of HR~6046\ on the plane of the sky as seen by {\it Hipparcos\/}\ is shown in
Figure~\ref{fig:hippath}.  The irregular pattern is the result of the
combination of annual proper motion (indicated by the arrow),
parallactic motion, and orbital motion.

\begin{figure}
\vskip -0.6in
\epsscale{1.3}
{\hskip -0.2in \plotone{f4.eps}}
\figcaption[]{Path of the center of light of HR~6046\ on the plane of the
sky, along with the {\it Hipparcos\/}\ observations (abscissa residuals)
represented as in Figure~\ref{fig:hiporbit} and
Figure~\ref{fig:deproject}. The irregular motion is the result of the
combined effects of the annual parallax, proper motion, and orbital
motion according to the solution described in the text.  The arrow
indicates the direction and magnitude of the annual proper
motion.\label{fig:hippath}}
\end{figure}

The detection of the photocentric motion by {\it Hipparcos\/}\ offers an
independent way of estimating the brightness difference between the
stars, in the passband of the satellite ($H_p$ band), from the
relation between the semimajor axis of the photocentric orbit and that
of the relative orbit in angular units \citep[e.g.,][]{vandeKamp:67}:
$a_{\rm phot} = a_{\rm rel}(B-\beta)$. Here $a_{\rm rel}$ can be
obtained from the spectroscopic minimum masses, the inclination angle,
and the parallax through Kepler's Third Law. $B$ represents the mass
fraction $M_{\rm B}/(M_{\rm A}+M_{\rm B})$, and $\beta$ is the light
fraction given by $L_{\rm B}/(L_{\rm A}+L_{\rm B}) = (1+10^{0.4\Delta
H_p})^{-1}$. The magnitude difference is then
\begin{equation}
\Delta H_p = 2.5 \log \left[ \left({q\over 1+q}-{a_{\rm phot}\over
a_{\rm rel}}\right)^{-1} - 1 \right]~,
\end{equation}
in which $q \equiv M_{\rm B}/M_{\rm A}$.  We obtain $\Delta H_p = 2.1
\pm 0.6$ mag, somewhat smaller but still broadly consistent with the
values in the Johnson $B$ and $V$ bands reported by \cite{Scarfe:07}
(see below), considering the difference in the passbands.

\section{Evolutionary status}
\label{sec:evolution}

From the analysis of their high-resolution spectra of HR~6046\
\cite{Scarfe:07} estimated the spectral types and luminosity classes
of the components to be \ion{K3}{2} and \ion{K0}{4}, and the
brightness difference to be $\Delta B \approx 2.5$ mag and $\Delta V
\approx 3.0$ mag. They then made use of the {\it Hipparcos\/}\ parallax (which we
now know is substantially correct) and the combined system brightness
to infer absolute visual magnitudes of $M_V = -0.68$ for the primary
and $M_V = 2.32$ for the secondary, ignoring extinction.  $U\!-\!B$
and $B\!-\!V$ color indices were computed by making use of standard
tabulated values for spectral types and luminosity classes close to
what they derived, along with the magnitude differences. The
photometry synthesized in this way provides a very good match to the
observed $B\!-\!V$ color of the system, and enabled \cite{Scarfe:07}
to claim that both stars are evolved, with the primary being near the
tip of the giant branch. They also pointed out that evolutionary
models by \cite{Pols:98} allow the brightness difference to be as
large as observed in HR~6046\ for component masses that differ by as
little as they do in this system ($\sim$1\%), at least for masses in
the most probable range for HR~6046, which they estimated to be 2.0--3.5
M$_{\sun}$. This provided a natural explanation for a set of
properties that had intrigued earlier investigators.

The minimum masses from the spectroscopic work of \cite{Scarfe:07}
combined with our inclination angle give absolute masses for HR~6046\ of
$M_{\rm A} = 1.38_{-0.03}^{+0.09}$~M$_{\sun}$ and $M_{\rm B} =
1.36_{-0.02}^{+0.07}$~M$_{\sun}$ (Table~\ref{tab:elements}), in which
the uncertainties are currently dominated by the error in $i$. These
masses are considerably smaller than assumed by those authors. We have
therefore re-examined the consistency with the evolutionary models by
making use of these values along with slightly revised absolute
magnitudes for the stars based on our new parallax. Given a distance
approaching 200~pc, a small amount of extinction would not be
unexpected for the system, and in fact the dust maps of
\cite{Schlegel:98} indicate a total reddening in the direction of HR~6046\
of $E(B\!-\!V) \sim 0.03$ mag. We tentatively adopt $E(B\!-\!V) \sim
0.02 \pm 0.01$ mag, which corresponds to $A_V \sim 0.06 \pm 0.03$ mag.
With this adjustment to the apparent magnitude $V = 5.63 \pm 0.01$
\citep{Haggkvist:87}, and taking into account the magnitude difference
from \cite{Scarfe:07} (to which we assign, somewhat arbitrarily, an
uncertainty of 0.3 mag), we infer individual magnitudes of $M_V^{\rm
A} = -0.62 \pm 0.20$ and $M_V^{\rm B} = 2.38 \pm 0.34$. These are not
changed much from the original estimates of \cite{Scarfe:07}.  The
$B\!-\!V$ colors proposed by them rely on an external tabulation and
are quite sensitive to the luminosity class adopted, so we have
preferred to proceed without them here, although they may well be
accurate. The models by \cite{Girardi:00} are a convenient choice for
a comparison with the observations, since they reach the late
evolutionary stages needed for the primary and are tabulated for a
wide range of chemical compositions and ages. They also incorporate
mass loss due to winds in the giant phase, which turns out to be only
a 1--2\% effect for HR~6046.

\begin{figure}
\vskip -0.4in
\epsscale{1.4}
{\hskip -0.35in \plotone{f5.eps}}
\vskip -0.25in
\figcaption[]{Model isochrones from \cite{Girardi:00} that match the
measured absolute magnitudes (grey areas) and current masses of HR~6046\
within the observational errors, shown for a range of metallicities
and ages as labeled. Open circles on each isochrone indicate the
expected location of the components, and the plus signs represent the
predicted system magnitude and color. The system magnitude and color
actually measured are represented by the filled circle and error
bar. The model drawn with the heavy line satisfies the additional
constraint given by the observed $B\!-\!V$ color of the system.
\label{fig:isochrones}}
\end{figure}

In Figure~\ref{fig:isochrones} we show several isochrones for
different metallicities from this series of models that produce the
best simultaneous match to the absolute magnitudes of both components
at their current masses (accounting for mass loss). In each case
(except for the middle isochrone) the age is the one providing the
best agreement among the values tabulated by \cite{Girardi:00}, which
come in steps of 0.05 in $\log t$.  The location of the stars on these
models is indicated with open circles. The combined color and
magnitude predicted for the system in each case is shown by the plus
signs, and the filled circle represents the measured values of $M_V$
and $B\!-\!V$ for HR~6046. The system color we have adopted is $B\!-\!V =
1.34 \pm 0.01$ \citep{Haggkvist:87}, which we have then dereddened as
indicated above.  Properties of the stars inferred from these models
are listed in Table~\ref{tab:models}. If we now impose the additional
requirement that the isochrones match the measured system color within
its uncertainty, a very good correspondence may be obtained by
interpolation for a metallicity of $Z = 0.011 \pm 0.002$
(corresponding to [Fe/H] $= -0.24 \pm 0.07$ for the assumed $Z_{\sun}
= 0.019$ in these models) and a logarithmic age of $\log t =
9.49_{-0.09}^{+0.04}$ (or $3.1_{-0.6}^{+0.3}$~Gyr). This model is
shown with the heavy line in Figure~\ref{fig:isochrones}, and
indicates that the primary is indeed approaching the tip of the giant
branch, whereas the secondary is beginning its first ascent of the
giant branch. We infer from this best-fitting isochrone that the
primary star has a radius of $30.9_{-1.1}^{+3.6}$~R$_{\sun}$, a
surface gravity of $\log g = 1.60_{-0.08}^{+0.04}$, and an effective
temperature ($T_{\rm eff}$) of $4211_{-23}^{+16}$~K, and the secondary
has $R = 4.20_{-0.33}^{+0.27}$~R$_{\sun}$, $\log g =
3.33_{-0.04}^{+0.07}$, and $T_{\rm eff} = 5010_{-47}^{+79}$~K. These
uncertainties account for all observational errors but exclude
possible systematics in the models.  Other properties of the stars for
this metallicity are listed in Table~\ref{tab:models}.

\subsection{Additional spectroscopic constraints}

With the goal of providing a check on the temperature of the primary
star, we obtained a high-resolution spectrum of HR~6046\ on UT 5 July 2007
using the HIRES instrument \citep{Vogt:94} on the Keck~I telescope.
The spectrometer slit was $0\farcs86$, giving a resolving power of
$\lambda/\Delta\lambda \approx 55,\!000$. The signal-to-noise ratio of
this spectrum is $\sim$120 per pixel. The spectral region
$\lambda\lambda$6200--6300~\AA\ was used to measure a number of
temperature-sensitive lines mainly of \ion{Fe}{1} and \ion{V}{1}, and
also a few of \ion{Ni}{1}, \ion{Sc}{1}, \ion{Si}{1}, and
\ion{Fe}{2}. As described by \cite{Gray:91} and others, line-depth
ratios (LDRs) of properly selected line pairs are an excellent
diagnostic of effective temperature that allow for \emph{relative}
measurements with a precision as small as a few K, not only in dwarfs
but also in giants \citep{Gray:01}.  The conversion to an
\emph{absolute} temperature scale, however, necessarily depends on an
external color-temperature calibration since LDR variations are
usually compared with corresponding changes in a color index such as
$B\!-\!V$, which is an easier quantity to measure than temperature.
Therefore, absolute temperatures are much less certain. We measured a
total of 26 lines of the primary star\footnote{The secondary is too
faint to affect these measurements, and would not influence them even
if it were brighter \citep[see][]{Gray:01}.} from Table~1 by
\cite{Biazzo:07}, and used their calibrations appropriate for giants
for 16 selected line pairs to derive an average temperature from the
LDRs of $T_{\rm eff} = 4340 \pm 20$~K (formal error).  The scatter of
the individual determinations is only 80~K. The color-temperature
relation on which the above calibrations are based is that of
\cite{Gray:05}, which combines dwarf and giant temperatures obtained
by many different methods. For this work we have preferred to rely on
a more sophisticated color-temperature relation such as that by
\cite{Ramirez:05}, which accounts not only for luminosity class but
also metallicity, and is based on effective temperatures derived
homogeneously by the Infrared Flux Method. The conversion from the
above LDR-based $T_{\rm eff}$ back to an average color for the primary
star was made using the same prescription by \cite{Gray:05}, and gives
$B\!-\!V = 1.328 \pm 0.014$. The \cite{Ramirez:05} calibration for an
adopted metallicity of [Fe/H] $= -0.24$ (\S\ref{sec:evolution}) then
yields $T_{\rm eff} = 4210 \pm 60$~K, in which the error combines
photometric uncertainties and the scatter of the calibration. This
result is in virtually perfect agreement with the temperature
predicted by the \cite{Girardi:00} models, supporting our overall
conclusions from the previous section.

\section{Discussion and concluding remarks}

The example of HR~6046\ is one of a growing number of binaries in which
the {\it Hipparcos\/}\ intermediate data have been brought to bear on the orbit of
the system, providing complementary information to that afforded by
other types of observations \citep[see, e.g.,][]{Pourbaix:04,
Fekel:05, Fekel:07, Torres:06, Torres:07a, Torres:07b}. In this case
the {\it Hipparcos\/}\ data yield the inclination angle, and allow the absolute
masses to be derived for the first time. Additionally they provide an
estimate of the brightness difference.

Although the inclination we derive for the orbit is consistent with
90\arcdeg\ and allows for the possibility of eclipses, chances are
slim because of the long period compounded by the relatively large
uncertainty in $i$. No photometric variability was found by
\cite{Percy:93}, who, however, apparently did not observe during the
eclipse phases, or by the {\it Hipparcos\/}\ satellite (scatter $\sigma_{H_p} =
0.007$ mag). The latter observations do straddle two of the eclipses,
which can be predicted very accurately from the spectroscopic orbit of
\cite{Scarfe:07} with errors of only 1.0 days for primary eclipse (HJD
$2,\!448,\!652.4$) and 1.4 days for the secondary (HJD
$2,\!448,\!419.3$).  If central, the eclipses would last approximately
18 and 22 days, respectively.  Examination of the epoch photometry
from {\it Hipparcos\/}\ indicates that both of these eclipses were missed by just a
few days. Future eclipses would be expected to occur at Julian dates
$2,\!455,\!254.7 \pm 1.2$ and $2,\!457,\!455.5 \pm 1.4$ for the
primary, and $2,\!455,\!021.6 \pm 1.4$ and $2,\!457,\!222.4 \pm 1.6$
for the secondary. The small separation of only 233 days (10.6\% of a
cycle) between the secondary eclipses and the primary events that
follow is due to a combination of high eccentricity and a longitude of
periastron near zero.

A second implication of the near edge-on orientation of HR~6046\ is
significantly lower component masses than previously assumed, which in
turn leads to a linear semimajor axis for the relative orbit of $4.63
\pm 0.11$ AU, corresponding to $26.0 \pm 2.4$ mas. The maximum angular
separation subtended by the binary is about 43 mas, also considerably
smaller than has been suggested in the past \citep[$\sim$70
mas;][]{McAlister:76, Halbwachs:81}. About two dozen unsuccessful
attempts to detect the secondary have been made over the past 3
decades with the speckle technique. Some of them were made at phases
in the orbit when the instrumental resolution should have allowed the
observers to resolve the pair, suggesting the large disparity in
brightness ($\Delta V \approx 3$) as the cause of those
non-detections. In principle the expected separations make it a good
target for long-baseline interferometry, except that in most cases
these instruments observe in the near infrared, where the brightness
difference will be even more extreme. From our modeling we expect
$\Delta J \sim 3.8$ mag and $\Delta K \sim 4.1$ mag. Still, some of
these facilities may have the sensitivity required. They could also
resolve the primary itself; the angular diameter should be
approximately 1.6 mas, while that of the secondary is only 0.2 mas.

Double-lined spectroscopic binaries with two giant components are a
relatively rare occurrence, and usually imply the components must have
nearly identical mass.  HR~6046\ is quite remarkable in that the stars
have attained a large brightness difference that is near the maximum
for this system, yet the secondary is still visible. Evolution
proceeds very rapidly at this stage, and according to the models the
difference in brightness may still increase by another half a
magnitude or so in $V$ over the next 20~Myr, which represents only
$\sim$0.5\% of its present age.

\acknowledgements

We are grateful to an anonymous referee for helpful suggestions on the
original manuscript.  Partial support for this work from NSF grant
AST-0708229 and NASA's MASSIF SIM Key Project (BLF57-04) are
acknowledged. This research has made use of the VizieR service
\citep{Ochsenbein:00} and of the SIMBAD database, both operated at
CDS, Strasbourg, France, as well as of NASA's Astrophysics Data System
Abstract Service. Alex Sozzetti is thanked for help in obtaining and
reducing the Keck spectrum of HR~6046.

redpajama_set_name: RedPajamaArXiv


Good food is a big part of any holiday. When you come to Krakow, we want to make sure you taste the best. From home-cook favorites to international and exotic, Krakow has a booming culinary scene that's sure to keep you satisfied.
Every good day starts with a good breakfast. And Zenit is one of the best places to get your early morning fill. The options are varied. Presently we suggest the French toast as it's both filling and oh so delicious. Not to mention the fact that every plate comes out looking like something you'd see on Instagram. Add a great coffee and a buzzing atmosphere and you'll probably find yourself spending a few hours here.
Ultimately if you're looking for the best of Poland, Starka is the place to go. Just a short hop from the enchanting Corpus Christi Basilica, the restaurant serves up some of the finest staples of Polish cuisine. It includes sour rye soup, their own signature salads, pork sirloin, and some mighty fine tasting desserts.
Also, check out the homemade flavored vodkas they have if you want the night to include a bit of a buzz.
If Italian is your thing then Mamma Mia do it right. Book ahead if you want a good table as the place is often packed. That's no surprise when you see the delicious range of pastas, pizzas and other snacks available at this place. In addition the wine list is equally as impressive. And the staff are on hand to ensure a good meal and a warm welcome to Krakow.
You can't come to Krakow and not go for the authentic Polish milkbar experience. These were the canteens that used to feed workers day in and day out during socialist times. Think no frills surroundings and a simple-yet-tasty menu.
However if you'd like to sip some fancy cocktails and take in the atmosphere around Szczepański Square, then Scandale Royal is the place for you. Other than the aforementioned beverages, the food is unpretentious and tasty (the breakfast comes particularly recommended) and the interior is cosy meets classy.
Finally, if Mediterranean is a must then check out Restauracja Pino. People rave about for its stylish comfy interior and the menu is full of tasty things like duck sous vide with sweet potato puree and ribs in tomato and honey sauce. Also being ever so slightly hip, this is also a great place to people watch the locals.


Mr. J. Mark Bottomley is Finance Director, Executive Director of Cranswick PLC. Mark, who is a chartered accountant, has extensive food sector experience, previously holding a variety of senior finance roles in the food production industry before joining Cranswick in 2008 as Group Financial Controller. He was appointed to the Board as Finance Director in 2009 and is responsible for overseeing the financial operation of the Group and setting financial strategy.


text:
Little Rock Culture Vulture
Cultural events, places and people in the Little Rock area
About the Little Rock Culture Vulture
Little Rock Cultural Institutions and Organizations (alphabetical)
LR Cultural Sites by Discipline
Shows Seen
NPHS Fall of the House of Usher, ushers in fall
PIPPIN's Magic Just for You
The Lullaby of a Golden Tent Season
Thoroughly Enjoyable Millie(s)
2014 Tony Award Predictions
2015 Tony Awards
2015 Tony Award Nomination Predictions
Tony Award Nomination Analysis
2016 Tony nomination predictions
Where's B? An appreciation of Byrne Blackwood
Tag Archives: The Accidental Tourist
Rock the Oscars 2019: Geena Davis
Posted on February 7, 2019 by Scott
On February 7, 2012, Academy Award-winning actor Geena Davis spoke in Little Rock. She was hosted by the University of Arkansas Clinton School for Public Service and the William J. Clinton Foundation.
Davis founded the Geena Davis Institute on Gender in Media in 2004. The institute is the only research-based organization working within the media and entertainment industry to engage, educate and influence the need for gender balance, reducing stereotyping and creating a wide variety of female characters in entertainment. Davis won the Academy Award for Best Supporting Actress for her role in "The Accidental Tourist" in 1988.
She was again nominated for an Academy Award and Golden Globe for her performance as Thelma in Ridley Scott's "Thelma and Louise," in which she co-starred with Susan Sarandon. She received a Golden Globe nomination for Best Actress for her portrayal of baseball phenomenon Dottie Hinson in "A League of Their Own."
Geena Davis is the founder of the non-profit Geena Davis Institute on Gender in Media and its programming arm See Jane, which engages film and television creators to dramatically increase the percentages of female characters — and reduce gender stereotyping — in media made for children 11 and under. In 2015, she founded the Bentonville Film Festival.
Posted in Film	| Tagged Academy Awards, Bentonville Film Festival, Clinton Foundation, Clinton School of Public Service, Clinton School Speaker Series, Geena Davis, Oscars, The Accidental Tourist
Rock the Oscars: Past Clinton School speaker Geena Davis
Geena Davis is not only an Oscar and Golden Globe winning actor, but a world-class athlete (at one time the nation's 13th-ranked archer), a member of the genius society Mensa, and is becoming recognized for her tireless advocacy of women and girls nearly as much as for her acting accomplishments. She is the founder of the non-profit Geena Davis Institute on Gender in Media and its programming arm See Jane, which engages film and television creators to dramatically increase the percentages of female characters — and reduce gender stereotyping — in media made for children 11 and under.
Davis is also a former trustee of the Women's Sports Foundation, serves on the Board of the White House Project, is an appointee to the California Commission on the Status of Women, and is an official partner of UN Women in their effort to change the way media represents women and girls worldwide.
Davis holds honorary degrees from Boston University, Bates College and New England College.
Posted in Film	| Tagged Academy Awards, Clinton Foundation, Clinton School of Public Service, Clinton School Speaker Series, Geena Davis, Geena Davis Institute on Gender in Media, Oscars, The Accidental Tourist, Thelma and Louise
Contact Little Rock Culture Vulture
Email me at lrculturevulture@aol.com
Send suggestions for features and items to be included in future posts.


text:
Страцин () — село в Болгарии. Находится в Бургасской области, входит в общину Поморие. Население составляет 1 306 человек.

Политическая ситуация
В местном кметстве Страцин, в состав которого входит Страцин, должность кмета (старосты) исполняет Хасан Иса Кралы (Движение за права и свободы (ДПС)) по результатам выборов правления кметства.

Кмет (мэр) общины Поморие — Петыр Георгиев Златанов (независимый) по результатам выборов в правление общины.

Ссылки
 Статистика населения

Сёла Бургасской области

redpajama_set_name: RedPajamaWikipedia


text:
Decoding Ukraine
A lexicon of the smears, stereotypes, and clichés used to describe the battle for the country's future.
By Anne Applebaum
Feb 20, 20148:00 PM
Anti-government protesters clash with police in Independence Square on Feb. 19, 2014, in Kiev, Ukraine.
Photo by Alexander Koerner/Getty Images
WARSAW, Poland—For those who are new to the subject—indeed, for those who have been following it for many years—the Ukrainian crisis can seem murky. The Ukrainians have a president, Viktor Yanukovych, who granted himself dictatorial powers and then repealed some of them, announced a truce and then broke it, and claims to enforce the law but employs thugs who haul journalists out of cars and shoot them. The Ukrainian opposition, meanwhile, has three separate leaders who may or may not actually control the Ukrainian protest movement at any given moment.
The opacity helps to explain why Ukraine, after years of stability, has suddenly become violent and unpredictable. It also helps to explain why so many inside and outside the country use historical clichés to describe the situation. Often, those clichés are intended to serve the interests of those who use them. Sometimes they are just bad simplifications. Either way, what follows is a handy guide to the terms, words, and phrases to treat with deep skepticism:
Fraternal assistance
This is a Soviet expression, once used to justify the Soviet invasions of Prague in 1968 and Afghanistan in 1979. Fraternal assistance was intended to prevent Soviet puppet states from being overthrown, whether violently or peacefully. In December, Russian President Vladimir Putin called Ukraine a "fraternal" country, hinting that he sees it as a puppet state. This week, a senior Russian parliamentarian declared that he and his colleagues are "prepared to give all the necessary assistance should the fraternal Ukrainian people ask for it." This may well be the cue for pro-Russian organizations inside Ukraine to ask for intervention.
Anti-terrorist operation
This is a Putin-era expression used to justify the Russian invasion of Chechnya in 1999. An anti-terrorist operation, in this particular context, means that anything is permitted: The term granted Russian soldiers carte blanche to destroy Grozny, the Chechen capital. This is why so many reacted with horror earlier this week when the Ukrainian defense ministry warned that the army "might be used in anti-terrorist operations on the territory of Ukraine."
Coup d'etat
This more universal expression has been used since November by both the Ukrainian government and Russian commentators to describe street protests in Kiev and elsewhere. It can mean anything from "peaceful protests that we don't like" to "protesters using violence against police," but either way, it is a term being used to justify the deployment of an "anti-terrorist operation" and not necessarily to describe an actual coup d'etat.
Nazi or fascist
These loaded historical terms have been used by both Russian and Ukrainian officials for many months to describe a wide range of opposition leaders and groups. Fake photographs of nonexistent Hitler posters in Kiev have been circulating online; recently, the Russian foreign minister lectured his German colleagues for, he said, supporting people who salute Hitler. Of course there is a Ukrainian far right, though it is much smaller than the far right in France, Austria, or Holland, and its members have indeed become more violent under the pressure of police clubs, bullets, and attacks.
At the same time, those who throw these terms around should remember that the strongest anti-Semitic, homophobic, and xenophobic rhetoric in this region is not coming from the Ukrainian far right but from the Russian press and ultimately the Russian regime. As historian Tim Snyder has written, "The Ukrainian government is telling itself that its opponents are Jews and us that its opponents are Nazis." The smears do stick. Romano Prodi, the former president of the European Commission, just wrote an otherwise anodyne article ticking off Ukrainian "far-right nationalist groups" as if they were the main problem, proving that even Western statesmen aren't immune.
Ethno-linguistic divisions or Yugoslav situation
These are more loaded terms, used in both the West and Russia, to show that the conflict in Ukraine is atavistic, inexplicable, and born of deep ethnic hatred. In fact, this is not an ethnic conflict at all. It is a political conflict and—despite the current opacity—at base not that hard to understand. It pits Ukrainians (both Russian and Ukrainian-speaking) who want to live in a "European" democracy with human rights and rule of law against Ukrainians (also both Russian and Ukrainian-speaking) who support an undemocratic, oligarchic capitalist regime that is politically and economically dependent on Russia. Some of the regime's supporters may well believe they are fighting fascists and militant European homosexuals; others may simply fear that deep reforms will cost them their paychecks.
Either way, this is not a fight over which language to speak or which church to attend. It is a deep, fundamental disagreement about the nature of the state, the country's international allegiances, its legal system, its economy, its future. Given how much Ukrainians have at stake, the least we outsiders can do is avoid foolish stereotypes when discussing their fate.
Foreign Policy International Russia


text:
Florida basketball score: Gators fall short as No. 10 Michigan State edges out tough win
December 8, 2018 | By Adam Silverstein
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November 23, 2018 | By Adam Silverstein
The Florida Gators' third game in the Bahamas looked a lot like their first — but worse — as they again went ice cold from the field in a 60-54 loss to...
Florida basketball score vs. Stanford: Gators split first two games in the Bahamas
Through two games in the 2018 Battle 4 Atlantis in Paradise Island, Bahamas, the Florida Gators have looked like two completely different teams. After struggling to score in a 65-60 loss to...
Florida basketball to play in 2019 Charleston Classic with UConn, Miami in field
Florida Gators basketball's 2019-20 schedule began to take shape on Thursday when it was announced they will be one of eight teams competing in the 2019 Charleston Classic. The event, held in...
Florida basketball score vs. La Salle: Gators roll again but have plenty of room to grow
As the Florida Gators continued to gear up for their holiday week trip to the Bahamas, some more home cooking was just what they needed. Florida (2-1) earned a decisive victory over...
Florida basketball score vs. Charleston Southern: Gators bounce back with rout at home
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Three days after being absolutely embarrassed in their season opener at No. 17 Florida State, some home cooking appeared to be just what Florida Gators basketball needed. Florida (1-1) blasted the Charleston...
Florida basketball vs. Florida State: Prediction, pick, line, spread, odds, watch live stream online
Unranked entering the 2018-19 season, Florida Gators basketball looks to continue its progression under head coach Mike White, who enters his fourth year with a team now filled with his recruits. Coming...
Florida basketball wins exhibition opener, but Mike White is none too pleased
October 31, 2018 | By Adam Silverstein
With a bevy of new players and flirting with the preseason top 25, Florida Gators basketball took the court for the first time on Tuesday in an exhibition game not available to...
Florida basketball schedule: Gators with three games on CBS Sports in 2018-19 season
CBS Sports released its 2018-19 college basketball schedule on Tuesday, and the Florida Gators will open the season as one of of the network's most prominently featured teams over the course of...
« First‹ Previous4567891011121314Next ›Last »
Schedule: Basketball 2019-20
Time/Score
TV/Rec.
11/5 North Florida W 74-59 1-0
11/10 Florida State L 51-63 1-1
11/14 Towson
Charleston Classic W 66-60 2-1
11/17 at UConn L 59-62 2-2
11/21 vs. St. Joe's
11/22 vs. Miami
11/24 vs. Xavier
11/29 Marshall W 73-67 6-2
12/7 at Butler L 62-76 6-3
12/17 vs. Providence
Naismith HOF Game W 83-51 7-3
12/21 vs. Utah State
Orange Bowl Classic L 62-65 7-4
12/28 Long Beach State W 102-63 8-4
1/4 Alabama 6 p.m. ESPN2
1/7 at So. Carolina 7 p.m. ESPN2
1/11 at Missouri 8:30 p.m. SECN
1/14 Ole Miss 7 p.m. ESPN
1/18 Auburn 1:30 p.m. CBS
1/21 at LSU 7 p.m. ESPN
1/25 vs. Baylor
SEC/Big 12 Challenge 8 p.m. ESPN
1/28 Miss. State 7 p.m. ESPN
2/1 at Vanderbilt 8:30 p.m. SECN
2/5 Georgia 7 p.m. ESPN2
2/8 at Ole Miss 2 p.m. ESPN
2/12 at Texas A&M 8:30 p.m. SECN
2/15 Vanderbilt 8 p.m. SECN
2/18 Arkansas 7 p.m. ESPN
2/22 at Kentucky 6/8 p.m. ESPN
2/26 LSU 9 p.m. ESPN2
2/29 at Tennessee 2 p.m. ESPN
3/7 Kentucky 1 p.m. CBS
Basketball: 2020 Class
Sam Ruzhentsev (107) F
Niels Lane (119) G
Osayi Osifo (5J) F
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Botswana, Okavango Delta, an alluvial plain, which in the period of full amplitude reaches 16,000 square kilometres out to become the second largest inland delta in the world.
The waters of this extensive water system originates from the north in Angola with the rains of October. From here begins a slow journey south. Instigated by the difference in height of 60 meters of 460 km, passing through Namibia, it takes about 9 months to reach the southern part of the Delta where there is the city of Maun, finally exhausting it's journey in the Kalahari desert.
This huge volume of water creates an incredible environment for plant and local animal life. There are many birds, both migratory that sedentary, inhabiting the Delta including eagles, herons and storks. Then of course there are in huge quantities the herbivores, who feast on the lush grass of January and reproduce there too. Antelopes, impalas, Wildebeest, large herds of buffalos, zebras, giraffes, warthogs and elephants to name a few. This abundance of herbivores inevitably attracts carnivores. Predators such as baboons, jackals, hyenas, lions, leopards and cheetahs.


What Does Walleye Taste Like? Surprising Answer You Need To Know!
→What Does Walleye Taste Like? Find Out the Surprising Answer You Need To Know!
There are many fishes in the sea (and the river!) that you can buy at the supermarket. You see a lot of them, mostly, in their filleted forms. You don't always see the whole fish in stores, except the smaller fishes. So, it's likely that you may not be familiar with how some fishes look at all!
What does walleye taste like? I think the better first question is what does walleye look like? How do you prepare walleye? If you are a fishing enthusiast, you might even want to catch one yourself! How do you fish for walleye? I'll do my best to answer all your questions!
Firstly, let me clear this up. Walleye is a freshwater fish, and it goes by many names. Depending on where you are, people have a local name for it. In Canada, it may be called pickerel, though they are not pickerels.
It's a close relative of the pikeperch and resembles its looks, but the two are distinct in color. Pikeperch is silvery from the belly and turns greenish approaching the dorsal fins. Walleyes, on the other hand, have golden scales and have rounder bellies.
What Does A Walleye Taste Like?
There will be a good debate on the taste of walleye. It seems that walleyes on different regions taste differently. But let's leave that to the connoisseurs and let's define what you may expect from a walleye. They come a bit expensive in restaurants and, I know, you at least want an idea how it tastes before getting one!
A walleye is a prized fish that you can easily prepare yourself. They yield a good amount of meat for their size. The best way to enjoy them, for me, is broiled or pan fried. Cooking it in other ways will add more flavor which may hide the distinct flavor of the walleye.
Well, some people say it tastes like chicken (maybe they were joking!). But a walleye tastes like a fish. It has a mildly fishy flavor. Some people may claim it's a bit bland and not as good as snappers. But fish meat is not just about the taste. The texture of walleye meat is top-notch!
Cooking it plainly will tell you the unadulterated flavor of walleyes. Pan frying them with some salt and pepper is already a mouthwatering feast! The texture is just astounding with a mild and satisfying distinct fish flavor!
But don't mistake walleye from Alaskan walleyes. They have the same name, and people get confused about it. Alaskan walleye is a saltwater dwelling fish and is not even a distant relative of the freshwater walleye.
Another simple way to prepare a walleye is to bake them. If you are not a fan of deep frying but want to have a similar taste, you can bake them to crisp!
If you can have whole walleyes, yes, the whole fish, with all the guts and everything that comes with a fish, you can make a tasty grilled fish dinner with it! Well, it may be a bit hard to find them in this form, but that shouldn't stop you from grilling your walleye!
Get a tin foil, spritz some nonstick spray, Season your fillet and grill it!
Who wouldn't love fishcake? Especially if it's made of walleye! Make this, and everyone will beg you for another serving!
If you are not a fan of eating raw fish, you may want to try a milder version of it. Milder regarding the rawness but full of flavor! Soaking fish in lime juice can cook it (not as cooked as you expect from deep frying it though!). It's a bit difficult to explain it, but you should try it!
If you have a fishing rod, and you live in the northern part of the US, and you like fishing, you better catch your walleye to enjoy it in its freshest form! Walleyes are nocturnal feeders. The best time to catch them is before the sun comes up and after the sun goes down.
Walleyes usually bite on live baits so be sure you have it! Just be patient and wait for a bite. In a few hours, you will be going home with some delicious fish! Roast them on a spit!
Walleyes are one of the most sought after and prized freshwater fish. That's the primary reason they are a quite expensive in restaurants. But what does walleye taste like? Well, I just hope you can imagine the description above! But, still, the best way to find out is trying them out! They surely taste awesome!