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Chicken Potholders
Posted February 1, 2022 1:12am UTC by designer
These zany little chickens definitely march to the beat of their own drums! They are fun, funky, unconventional, and will make a welcomed addition to anyone's kitchen décor. They are made double thick from 100% cotton yarn so they are not only cute to look at, but functional as well. They measure approximately 8 1/2 inches across. These are available in the link below…
Donna Shepherd on February 1, 2022 at 1:29 am said:
I've clicked on every available button & cannot find the instructions for these chicken potholders. Thanks b
Nina on February 2, 2022 at 5:22 pm said:
The ad was covering it. I found "Find it HERE" under it…
https://www.etsy.com/listing/158723591/crochet-pattern-for-the-swanky-chicken?zanpid=10723_1643822481_0b1b56b67f306c903d55f3590866d5a4&utm_medium=affiliate&utm_source=affiliate_window&utm_campaign=eu_buyer&utm_content=349183&awc=10723_1643822481_0b1b56b67f306c903d55f3590866d5a4
Sandy Hurlbert on February 1, 2022 at 2:24 am said:
Awesome pattern how do I get the pattern? I can't find a link on your site for it…….
Thank youi
Denise Draeger on February 1, 2022 at 11:18 am said:
Judy ONeil on February 1, 2022 at 12:08 pm said:
These are adorable.
Cheryl Boyer on February 1, 2022 at 12:46 pm said:
Please send me info on the potholders
Barrett on February 1, 2022 at 2:12 pm said:
cute, would like to make
Bond Perry on February 1, 2022 at 3:00 pm said:
I am looking for the link to the chicken pot holders…..cant seem to find it…I get a parm cheese link
Sheila on February 1, 2022 at 7:49 pm said:
L Dering on February 1, 2022 at 8:58 pm said:
Please send details, price, etc about the Chicken potholders. Are they knit or crochet?
And how to purchase if other details ok with me. Thanks
Shirley Gipson on February 2, 2022 at 2:16 am said:
Very cute! How much are your potholders please? Thank you!
Emily Whitaker on February 2, 2022 at 3:08 am said:
No link found.
Eugenia Anderson on February 2, 2022 at 3:11 am said:
Hope I win !!!
Lise Pigeon on February 2, 2022 at 12:23 pm said:
Elles sont magnifiques
Valarie Lyles on February 2, 2022 at 1:45 pm said:
Please send pattern for chicken potholders
Carol Windham on February 2, 2022 at 4:50 pm said:
https://www.awin1.com/cread.php?awinmid=10723&awinaffid=349183&ued=https%3A%2F%2Fwww.etsy.com%2Flisting%2F158723591%2Fcrochet-pattern-for-the-swanky-chicken
albertbucklin Bucklin on February 3, 2022 at 1:32 am said:
cant find the dircetions. please tell me how to get thederictions thanks
Glenda Wittner on February 3, 2022 at 1:51 am said:
Need this to make! Cute
Sherry on February 3, 2022 at 3:13 am said:
UNDERNEATH the photo of the chicken potholders is a blue Open button. Right underneath that it says: Find it HERE. Click on the word "here". It's a $5.00 pattern on Etsy.
See my comment below. 😊
Daniele Brasington on February 3, 2022 at 7:16 am said:
I would love to have this pattern. Could you please send it to me. Thank you!
robyn on May 20, 2022 at 10:43 pm said:
so cute! please send pattern!


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Q: How to use regex to replace a string of symbols I am using regex in VsCode to replace the symbol * by the symbol # in the following situation:
* one
** two
*** three

by
# one
## two
### three

I was using [*] and [\*]{3}\s without coming to a solution.

A: You may use
Find What: \*(?=\**\s)
Replace With: #
See the regex demo online.
Details

*

*\* - a * char

*(?=\**\s) - a positive lookahead that requres 0 or more * chars followed with a whitespace immediately to the right of the current location.

See the VSCode demo:

After clicking Replace all:

redpajama_set_name: RedPajamaStackExchange


Lost City of Omu is the 13th major module release of Neverwinter. It continues the story in Chult by extending the Module 12 campaign and letting players explore the lost city before taking on Acererak and his Atropal in a new 10-character trial.
The update focuses on Masterwork Professions, gear upgrades and the Hunts system. It also features a lot of quality-of-life changes and balancing passes for the Scourge Warlock and Trickster Rogues.
Expedition Leader Pack: Is It Worth It?


the bistoury, the deeper muscular fibers separated with the fingers.
certain parts, as in pyloric or cardiac insufficiency.
splendid example, cheerfulness and courage that a great number of lives were saved.


Shipping Policy | Try Natural Living|Natural and Organic Products for Everyday Life.
ll orders are shipped directly from the supplier. The length of time it will take to arrive depends on the production time of the designer. Most orders ship within 3-4 business days. If ship time is longer than the average 7 days it will be listed in the product descriptions. Please expect to add 2-3 days for holiday orders. Some products will be charged an extra shipping surcharge.
*Currently we only ship to the continental United States.
If you need an order rushed, please contact us and we can make arrangements to get your order to you as soon as possible, based on the designer's inventory and policies.


We know how important it is to be able to socialise with those who have similar interests. The group provides a welcoming and relaxed atmosphere for adults with autism who are keen to meet other people who may experience similar social difficulties and integrate with others in a safe, social environment.
Our Interests Group was launched by a group of adults with autism for just that reason. On the last Sunday of every month, the group takes part in a new activity together. With interests in photography, gaming, petanque, archery and much more, they are certainly kept busy learning new skills and doing what they love. For more information please email [email protected].


text:
import sys
import inspect

def get_default_args(function):

    if sys.version_info < (3, 0):
        # The slightly hacky Python 2.7 way
        argspec = inspect.getargspec(function)
        default_args = dict(list(zip(
            argspec.args[-len(argspec.defaults):], argspec.defaults)))

    else:
        # The better Python 3 way
        sig = inspect.signature(function)

        default_args = {}
        for parameter in sig.parameters:

            default_val = sig.parameters[parameter].default
            if default_val is not inspect.Parameter.empty:
                # Add it to the parameter list
                default_args[parameter] = default_val

    return default_args

redpajama_set_name: RedPajamaGithub


I think in the future I can use Digital Ocean's API to launch as many seed nodes as we want for the first few days. This should make DAC launches as smooth as possible and not have everyone scrambling for seeds at launch or slow block downloads.
Can someone find or post a single run bash script to compile and run Protoshares from source? Should auto-generate a random rpc user and pass, and increase max connections.
Once that is done I can host it on Protoshares.com and automatically launch at least 3 permanent seednodes at my expense.
To make DAC launches easier I can probably launch temporarily ~50 seed nodes, but I need a script that takes out all the manual work first.
here's what happens when I take my node down for 30 minutes, guess what my block total is?
Pls to join Primedice 3 and frolic about merrily whilst gambling awe-inspiring quantities of bitcoins. The power of Christ compels you.
I have a dogecoin p2pool at Nogleg.


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Social Anxieties: Outdated sex education must be reformed at the federal level
By NATHANIEL HYMAN
November 27, 2018 in Columns, Opinion
My high school has a program called "Teen Pep," which features upperclassmen performing wacky skits to promote safe sex and STI prevention.
I disliked the program because one of the five seminars was titled "Postponing Sexual Involvement." In fact, I disliked it so much that I wrote an article for the school's satirical newspaper titled: "Teen Pep to Take Over Driver's Education, Dedicate Curriculum to 'Postponing Vehicular Activity.'"
I was too judgmental. Teen Pep made a respectable effort to educate students about both preventative and remedial birth control and STI protection.
Additionally, there isn't anything wrong with partially promoting abstinence; it's the most effective form of birth control and STI prevention. Excessive or exclusive promotion of abstinence is where sexual education starts to fail.
When considering what topics should be taught in sex ed, it's important to understand that teenagers are going to have sex. They are going to have sex regardless of whether they are taught safe sex, and they are going to have sex even if they promise otherwise. According to the National Center for Health Statistics, more than half of U.S. teenagers have sex by age 18, and according to a study by researchers at the University of Massachusetts at Amherst, over half of teenagers who pledge celibacy have sex before marriage and have a higher rate of STI contraction and premarital pregnancy than those who don't pledge.
Though it is important to remember that correlation does not imply causation, these statistics help explain why a joint study between Indiana University and the University of Georgia found that the more a state's sexual education curriculum focuses on abstinence, the higher its teen pregnancy rate. The study's findings were consistent even when controlled for socioeconomic factors such as household income and race.
But these socioeconomic factors are critical to understanding how teenage pregnancy disproportionately harms already disadvantaged populations. According to the National Campaign to Prevent Teen and Unwanted Pregnancy, 48 percent of teen mothers live below the poverty line, and 67 percent of teen mothers who move out of their own families' home live in poverty. Teen parenthood is the most common cause of girls dropping out of school, with approximately 50 percent of teen mothers never graduating from high school and less than 2 percent obtaining a college degree by age 30.
These socioeconomic impacts carry all kinds of long-term and cyclical consequences. According to the Schuyler Center for Analysis and Advocacy, children born to teen parents are nearly three times as likely to be incarcerated at a young age than the children of older parents, and the daughters of teen parents are 22 percent more likely to become teen mothers themselves.Effectively, teen pregnancy is a result of poverty, which can lead to crime, more poverty and, ultimately, more teen pregnancy. It's a vicious cycle, and the consequences predominantly affect the country's most vulnerable communities.
Yet, there is reason for hope. Teen pregnancy is dropping at an impressive rate, and that can largely be accredited to the increasing presence of "comprehensive" sexual education as opposed to abstinence-only education, a trend that has received scrutiny from the Trump administration.
In 2010, Congress created the Teen Pregnancy Prevention Program, which aims to fund organizations focusing on comprehensive sexual education. But in 2017, the Department of Health and Human Resources tried to remove funding from TPPP organizations to favor other, more conservative programs that emphasized "abstinence until marriage."
Fortunately, in April, a federal judge in the state of Washington issued a permanent injunction ordering the administration to continue funding the program, marking the second time a federal court had to make this order.
The effects of teen pregnancy, and the effects of abstinence focused sexual education are too well documented and understood for this to be just another trench battle in the endless culture war. We now know that time spent scaring teenagers away from sex entirely can be better used teaching them how to have safe sex, and the correct course of action isn't to remove funding from effective programs, but the answer also isn't to just fund individual comprehensive sex-ed programs.
There is currently no federally mandated sexual education curriculum, which has led to 26 states mandating that abstinence be stressed in public schools, and 11 states not having any mandated sexual education at all.
Studies have shown repeatedly that the less stress put on abstinence, the better the outcomes, regardless of location. So if lawmakers truly want to increase economic mobility, reduce crime and empower women, they must push for a federally mandated comprehensive sexual education curriculum.
Teenage pregnancy is becoming less and less of a problem in every regard. It's time to capitalize on the momentum that educators have built, not go back to the archaic philosophies that enabled the problem in the first place.
Nathaniel Hyman is a sophomore majoring in public policy. His column, "Social Anxieties," ran every other Tuesday.
EDITORIAL BOARD: Again, USC proves it prefers continuity over change Internet Cultured: Was the life of the 'influencer' really for ...

redpajama_set_name: RedPajamaCommonCrawl


text:
Home > Army > U.S. Army Patches > Army Patches Page 2 > Army Patches Page 3 > 173rd Airborne Brigade Patch
173rd Airborne Brigade (Sky Soldiers) Patch
173rd Airborne Brigade Patch
The shoulder sleeve insignia was originally approved on 13 May 1963.
The bayonet is used to refer to the brigade being borne by the wing alludes to the brigade's airborne status. Red, white and blue are the national colors.
Campaigns: World War II and Vietnam.
Decorations: Presidential Unit Citation- Army, Meritorious Unit Commendation- Army, Republic of Vietnam Cross of Gallantry with Palm, Republic of Vietnam Civile Action Honor Medal- First Class.
Our 173rd Airborne Brigade Army patch is a regulation, full color, embroidered military patch. This is the same patch that is supplied to the U.S. Army, Army National Guard, Army Reserve units, and sold in the Army Post Exchanges. This patch would be a great gift idea and a wonderful addition to your patch collection.


text:
Data/statistics (12)
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Migrant workers (3)
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Iran, Islamic Republic of (1)
Economic Commission for Africa (ECA) (3)
African Union Commission (2)
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Office of the United Nations High Commissioner for Human Rights (OHCHR) (1)
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Gender equality attitudes study (1)
Summary of 2022 preliminary results: UN Women Ethiopia strategic note 2021-2025
UN Women together with the Government through the Ministry of Women and Social Affairs (MoWSA) have significant advancements towards new policy developments and /or revision of the existing ones to match with the developments in the country.
UN Women Uganda Quarter 3 Newsletter July to September 2022
Date: Tuesday, 1 November 2022
This quarterly newsletter profiles UN Women Uganda activities and highlights voices of beneficiaries. The Q3 Newsletter covers the period of July to September 2022. Enjoy the read!
Collaborative on Administrative Data - Overview of the CAD
Administrative data collected by governments and service providers in their day-to-day business is an increasingly important source of official statistics. In the data revolution era, administrative data provides opportunities for timely analysis and public policy development, savings on data collection, and increased efficiency and scope using available data e.g., birth and employment records.
The Status of NEET. A quantitative analysis of A Quantitative Analysis of Youth Not in Employment, Education or Training (NEET) (15 – 24 years old)
Date: Friday, 7 October 2022
Since the onset of the COVID-19 pandemic and associated worldwide economic decline, East and Southern Africa (ESA) has suffered job losses and an increase in poverty, interruptions in healthcare services, and declined nutrition levels. Young adults whose place in the labor market is often informal, temporary, and tenuous at best have suffered greater job and income losses than their parents. As part of ensuring that recovery efforts also reduce the number of youth, young women, not in employment, education, or training (NEET), UN Women in ESA commissioned a quantitative study on the NEET status of youth aged 15-24 years in nine countries in the region. This report summarizes country findings and provides detailed analysis of available NEET data for youth aged 15-24 years with a view to supporting evidence-based policy advocacy and action in this area. This study covers Botswana, Ethiopia, Kenya, Malawi, Mozambique, Namibia, Rwanda, South Africa, and Uganda.
Policy Brief: Beyond Land Registration: How to support rural women to derive The full range of benefits from land in Ethiopia
Date: Wednesday, 5 October 2022
There is a tendency to view the sheer volume of land certificates issued in Ethiopia in recent years as a proxy for improvements in women's land tenure security. While getting land registered in women's names is a significant step, evidence indicates that focusing on titling alone may not necessarily lead to greater tenure security for women. Control and transfer rights of land for women are affected by broader gendered norms and practices. It is high time to think more deeply around the post-certification agenda so that women can derive the full range of benefits from their land resources.
Minimum Set of Gender Indicators for Africa
Date: Thursday, 29 September 2022
The purpose of the Global Minimum Set of Gender Indicators is to develop a common statistical measurement framework that could be used for the national production and international compilation of gender statistics and to track progress across countries and regions.
Africa Programme on Gender Statistics (APGS) Phase III Strategic Plan (2022-2026)
Date: Friday, 23 September 2022
Lack of adequate data to inform and monitor policies and progress undermines efforts to move forward Africa's gender agenda. The production of gender statistics in the region has been slow due to a combination of factors discussed in this Plan. However, increased interest in gender statistics and the current conducive policy environment for the their integration into statistical databases provide valuable opportunities to further strengthen statistical systems in Africa.
Guidance Note Integrating a gender perspective into implementation of Agenda 2030
This study explains why it is important to integrate a gender perspective into assessments of all the SDGs, and also shows how to approach this task as a way to enhance gender mainstreaming across the 2030 Agenda.
Gender Analysis Toolkit for Prioritising SDG Goals and Targets How to improve the knowledge base for SDGs, remove gender gaps in evidence, and integrate gender perspectives into analyses of SDGs
Consistent integration of a gender perspective into each SDG requires that the methodological approaches used to analyse targets should be capable of identifying gender inequality concerns in the 'gender silent' targets and when mapping interlinkages between them. Ths toolkit adresses sustinability issues by providing SDG researchers, analysts, and policy experts with the necessary tools to incorporate gender considerations throughout their Agenda 2030 related work.
UN Women Kenya Annual Report 2021
UN Women Kenya Annual report shares results and lessons learned for 2021.
UN Women Uganda Quarter 2 Newsletter 2022
This quarterly newsletter profiles UN Women Uganda activities and highlights voices of beneficiaries. The Q2 Newsletter covers the period of April to June 2022. Enjoy the read!
Quantitative Analysis of Youth Not in Education, Employment and Training (NEET) 15–24 years old |Regional Report
Date: Wednesday, 25 May 2022
The study covers Botswana, Ethiopia, Kenya, Malawi, Mozambique, Namibia, Rwanda, South Africa, and Uganda. It finds that NEET rates in ESA are above 40 percent for youth in the 20-24 years age bracket, that young women in the region are disproportionally affected by NEET status regardless of their age group, and that this status is more likely to become a permanent state for young women than for young men.
Youth Not in Employment, Education or Training (NEET) in East and Southern Africa - Summary of Key Findings and Policy Recommendations
NATIONAL SURVEY ON VIOLENCE IN UGANDA QUALITATIVE REPORT
The qualitative component of the Women's Health and Life Experiences study was designed to complement the larger survey on prevalence which seeks to generate reliable estimates of the prevalence of different forms of Violence Against Women and girls (VAWG), provide detailed information on the impacts of VAWG, and examine women's attitudes to violence, how women cope with violence, and the risk factors associated with VAWG. It provides contextual information on women and community perspectives and experiences of Violence against women and girls (VAWG).
Gender Alert on Drought in Ethiopia
The current drought response in Ethiopia is being scaled up across sectors, including food security, nutrition assistance, provision of safe water and sanitation, and livelihood protection. In addition, other urgent humanitarian assistance to drought- stricken areas such as agriculture and livestock support for pastoralist communities are also being increased. Nonetheless, the needs of women and girls may not be met due to a number of compounding factors such as the breakdown of key services which are critical to the health, protection, and recovery of women and girls; weakened informal and formal protection and accountability mechanisms; disrupted livelihoods, increased displacement, power imbalances, and limited access to resources.
UN Women in Zimbabwe Highlights from 2020-2021
Date: Tuesday, 19 April 2022
The Annual Report captures the work of UN Women in Zimbabwe to accelerate Gender Equality and Women's Empowerment in Zimbabwe. It highlights the organisation's initiatives, challenges and milestones achieved in 2021.
Assessment of gender data and capacity gaps in the national statistics system of South Sudan
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In Brief: Gender Statistics, Regional Office for East and Southern Africa
Date: Thursday, 6 January 2022
This brief gives an overview of the Gender Statistics programmes across East and Southern Africa.
Malawi National Gender Statistics Assessment
Date: Friday, 17 December 2021
The study identifies a number of challenges including inadequate normative frameworks and infrastructure to support statistical production, large time gaps between household surveys and censuses, limited dissemination and use of gender data and statistics across the NSS, and weak administrative data quality and systems in Malawi.


Condolence: Billy, I am so sorry to hear about the passing of your father. You and your family have my condolences. Take care. I know how you feel. But it's nice to know that he's alive up in heaven. That's what keeps me going.
Condolence: We met as kids in Mangla, West Pakistan. Jeff's brother, Joel, was my age and we were good friends. I recall his family as being very loving and kind.
He lived a full life and that is good. God bless him and his loved ones.
Condolence: Dear Carol...please accept our heartfelt condolences as you, family, and friends grieve the loss of Jeff, our dearly beloved brother in Christ. Our family was blessed by knowing Jeff as his zest for life, country, and most importantly his love of Christ touched our hearts in ways only Jeff could. May the hope of heaven bring you peace and comfort that only God can provide in the days ahead.
Condolence: My condolences to you Carol and to all of Jeff's blood family as well as all his many "brothers and sisters." I met Jeff (and Carol) back when I traveled to Irving regularly from Massachusetts on business. Jeff and I called each other "brother," and we meant it. Jeff demonstrated honesty, accountability and service to others. He spoke the truth in love. He told you what you needed to hear and not necessarily what you wanted to hear. My travels to Irving will never be quite the same without Jeff there to make me laugh, bust my chops, and inspire me to be a better person. I will always miss you, my brother.
Condolence: My condolences Mrs. DiGangi. Many happy memories be with you. And may these promises from Jehovah God comfort you now, and in the days to come. "Do not be anxious….but in everything by prayer and supplication along with thanksgiving, let your petitions be made known to God; and the peace of God that surpasses all understanding will guard your hearts and your mental powers by means of Christ Jesus." Philippians 4:6-7; Isaiah 25:8 NWT.
Condolence: Dear Carol and family, I am so sorry this passing has occurred. Jeff was funny and very polite to me over the years. What a loss for all of you, including our program.
I am sorry that I will miss the memorial since I am taking my grandchildren to Florida that week.
My thoughts are with you Carol.
Condolence: Our deepest condolences Carol and Family. What a special, wonderful guy! Jeff, we are so happy to have known you. Talitha and Elijah also send their love.
Condolence: May you Rest In Peace Jeff. I hope that your family is comforted by their faith and their friends and a presence of our loving God.


A retro, pixeljam version of the Robot Unicorn Attack game. Your favorite unicorn is back to eat magic stars and poop rainbows. Retro Unicorn Attack features. Chase your dreams and see if your wishes come true! Run and jump as you try to collect bonus unicorns and dash through stars on your way. Are you in for a. Play Retro Unicorn Attack - Journey all the way through the kingdom of wonders, with retro graphics it is funky yet fabulous!.
28 Sep Retro Unicorn Attack, a free online Arcade game brought to you by Armor Games. Our favorite running unicorn is back in an all-new all-old web. Robot Unicorn Attack. Play your favourite game without ads and boring loading screens. Robot Unicorn strikes back, this time in the awesome, 8-bit oldschool looking version. Run as far as you can, jump over deadly chasms and dash into your.
4 Dec - 2 min - Uploaded by Adult Swim Our favorite running unicorn is back in an all-new all-old web game! Turn back the clock to a. Play as a unicorn and chase your dreams in this retro version of Adult Swim's Robot Unicorn Attack. Jump over gaps to avoid falling to your death and use your . Robot Unicorn Attack - A Free Online Flash Game From Adult Swim. Click this; listen to the song; play the game. Trust us. Watch your favorite unicorn eat magic stars and poop rainbows in Pixeljam's retro version of the Adult Swim classic. Now with challenge stages and other. Robot Unicorn Attack is an online "endless running" video game featured on the Adult Swim and Flashline Games website. The game was produced by.
6 Jun Kongregate free online game Retro Unicorn Attack - Watch your favorite unicorn eat magic stars and poop rainbows in Pixeljam's retro version. Retro Unicorn Attack: Challenge Edition, Join this magical creature on an adventure that's a blast from the past. Robot Unicorn Attack: Heavy Metal, Join this mighty steed as she blazes through a dark world filled with chaos, fire, and some rad metal music. Rate: 70% (96 Votes). Robot Unicorn Attack: Heavy Metal; Romantic Pursuit; Canabalt; Unicorn Attack; Run Raptor Rider; Cyber Rush; Steel Jack.
12 Apr Imagine then our appreciative, wistful sigh upon learning of PixelJam's new game with Adult Swim, Retro Unicorn Attack: Challenge Edition. 30 Dec Like a comet made of gold, glitter and Lady Gaga's eyelashes, Robot Unicorn Attack circled the Earth and filled the firmament with its irresistible. Robot Unicorn Attack is a free Flash game from [adult swim]. You're a rainbow- adorned robot unicorn who runs across a pink, sparkly, brightly colored world . Sequel of the game, with a deliberately kitsch spirit and a girly universe, which was a huge success in Lead a unicorn with only 2 keys (Z: jump.


The awards for categories based on Global Custodian's mutual and hedge fund administration surveys will be presented at the Industry Leaders awards on 30 November in New York City.
Global Custodian has announced the nominations for awards categories based on its Mutual Fund Administration and Hedge Fund Administration surveys.
The awards will be presented at this year's North America Industry Leaders awards on 30 November at the Lighthouse, Chelsea Piers in New York City.
Both US Bancorp and Atlantic Fund Services are nominated for three categories within the MFA awards, while Deutsche Bank Fund Services and Opus Fund Services are up for two HFA awards each.
For full details of the Industry Leaders Awards event, including the GC sessions, please click here.


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text:
Feisty clipper Friday: Sharp snowfall gradient across Minnesota.
Photo: MPR
By Paul Huttner of Minnesota Public Radio News - January 14, 2021
Buckle up anywhere west of the Twin Cities Friday.
Our inbound Alberta clipper looks feisty. I give this storm a 7 on a scale of 1 to 10 for snow and wind potential Friday anywhere west of the Twin Cities.
Winter storm warnings expanded
The Twin Cities National Weather Service office expanded winter storm warning a couple of counties eastward Thursday afternoon. The warning zone basically includes all of Minnesota west of the Twin Cities.
Including the cities of Morris, Madison, Benson, Montevideo, Granite Falls, Redwood Falls, New Ulm, St James, and Fairmont
235 PM CST Thu Jan 13 2022
...WINTER STORM WARNING REMAINS IN EFFECT FROM MIDNIGHT TONIGHT TO MIDNIGHT CST FRIDAY NIGHT...
* WHAT...Heavy snow expected. Total snow accumulations of 7 to 10 inches.
* WHERE...Portions of south central, southwest and west central Minnesota.
* WHEN...From midnight tonight to midnight CST Friday night.
* IMPACTS...Travel could be very difficult. Patchy blowing snow could significantly reduce visibility. The hazardous conditions could impact the morning or evening commute.
Winter weather advisories include the southwest half of the Twin Cities. We could literally see a snowfall gradient from zero to 1 inch far northeast, to 5 or 6 inches in the far southwest Twin Cities.
Including the cities of Long Prairie, St Cloud, Monticello, Minneapolis, Chanhassen, Chaska, Victoria, Shakopee, Hastings, Faribault, Red Wing, and Owatonna
...WINTER WEATHER ADVISORY IN EFFECT FROM MIDNIGHT TONIGHT TO MIDNIGHT CST FRIDAY NIGHT...
* WHAT...Snow expected. Total snow accumulations of 1 to 5 inches.
* WHERE...Portions of central, east central, south central and southeast Minnesota.
* IMPACTS...Plan on slippery road conditions. The hazardous conditions could impact the morning or evening commute.
Snow coverage increases overnight
Snowfall is on track to increase from the Red River valley into western Minnesota in the wee hours after midnight Friday. Light snow likely pushes into the Twin Cities between about 6 a.m. and 9 a.m. Friday morning.
Notice how the northeast Twin Cities is literally on the edge of the snow:
NOAA NAM 3 km model between 3 a.m. and 6 p.m. Friday. NOAA via tropical tidbits
Sharp snowfall cutoff near Twin Cities
These systems often feature dry air eating away at the northeast edge of the snow zone. That typically produces a sharp snowfall gradient on the northeast edge of the storm.
That's why we could see an incredible snowfall gradient with little snow in the northeast Twin Cities, to as much as 5 or 6 inches in parts of Carver County in the far southwest Twin Cities. We could see a foot of snow in parts of southwest Minnesota.
Snowfall projection. Twin Cities National Weather Service
Factor in snow and wind to your Friday travel plans. Travel will be increasingly difficult as you move west and south of the Twin Cities.
Stay safe, Minnesota.
To see weather updates for Minnesota, follow this link to the MPR News website. https://www.mprnews.org/story/2022/01/13/feisty-clipper-friday-latest-model-project-sharp-snowfall-g...


text:
from b import *

def g():
    return f()


A Broward Sheriff's Office deputy was involved in a car crash early Monday morning near Pompano Beach.
According to BSO, Sgt. Brian Miller was headed southbound on I-95 in an unmarked BSO unit when he struck a Honda Civic that was stopped in the HOV lane, just south of Copans Road around 4:10 a.m.
Sgt. Miller, along with two adults in the other vehicle, were taken to Broward Health North hospital. Their injuries are non-life threatening.
It is not known why the Honda, driven by 29-year-old John Lewis of Coral Springs, was stopped in the HOV lane without any warning lights activated.
Sgt. Miller is a 29-year veteran with BSO.


text:
\section{Introduction}

A basic contradiction exists in the interpretation of [O/Fe] and [Mg/Fe] trends in
the Galactic bulge (McWilliam \& Rich 2004; Fulbright et al. 2007).  The [O/Fe]
ratio declines steeply with increasing [Fe/H], while the [Mg/Fe] ratio is enhanced in
all bulge stars, and only declines slightly by [Fe/H]$\sim$$+$0.5 dex.  An often used
paradigm (e.g. Tinsley 1979, Greggio and Renzini 1983, Matteucci and Greggio 1986)
to explain the alpha-element trend with metallicity, asserts
that the [O/Fe] ratio declines with [Fe/H] due to the addition of Fe from Type~Ia
supernovae (SNe) on long timescales.  Since Mg and O are thought to be produced in similar
mass (the most massive) progenitors of Type~II SNe (e.g. Woosley \& Weaver 1995;
henceforth WW95), it is expected that [O/Fe] and [Mg/Fe] should exhibit the same
trend with [Fe/H].  Thus, within this alpha-element paradigm the [O/Fe] trend suggests a
longer formation timescale for the bulge than does the [Mg/Fe] ratio.   McWilliam \& Rich (2004)
suggested that the steep decline in [O/Fe] was actually due to metallicity-dependent winds,
and related to the Wolf-Rayet phenomenon, rather than the addition of Fe from Type~Ia SNe.

In a previous paper (McWilliam  et al. 2008) we analysed the trend
of the [O/Mg] ratio in Galactic disk and bulge stars.
The observational data indicated that the [O/Mg] showed the same decline with increasing [Mg/H]
in both the bulge and disk, despite the very different formation timescales of these two systems,
and qualitatively consistent with metallicity-dependent O yields.  In
the McWilliam et al. (2008) paper we included
yields for oxygen from massive stars with metallicity-dependent winds
in detailed chemical evolution models for the bulge and
disk of the Milky Way.  In particular, we adopted the Maeder (1992) yields for
massive stars including mass loss; these yields are a strong function of the
stellar mass for stars at solar metallicity and above. For masses larger
than 25$M_{\odot}$, the oxygen production is strongly depressed as a consequence
of this mass loss.  In the presence of a strong mass loss during the Main Sequence phase
of massive stars, a larger amount of He and C are lost relative to stars evolving
at constant mass. This fact produces two main effects: i) a larger production of
He and C from stars with high metal content, ii) a smaller production of oxygen,
due to lack of C which is lost instead of being transformed into O.
In Maeder(1992) and Meynet \& Maeder (2002) this yield effect is important only
for the Z=0.02 models, while the yields of C and O from massive stars
with metallicities of Z=0.004, and below, do not differ substantially from the
yields computed without mass loss (e.g. Woosley \& Weaver 1995). This is due to the
fact that mass
loss in massive stars is a strong function of metallicity.  In McWilliam et al. (2008)
we showed that
the trends of [O/Mg], [Mg/Fe] and [O/Fe] in Galactic bulge and disk stars can be well
reproduced by models with the metallicity-dependent yields of Maeder (1992).
If these metallicity-dependent yields from massive stars are correct, then
the expectation is that the oxygen decline to higher metallicity
stars in the bulge, as evidenced by [O/Mg] and [O/Fe] trends, should be accompanied
by an increase in the [C/O] ratio.  Thus, the [C/O] ratio in the bulge provides a
test for the conclusions of McWilliam et al. (2008).  We note that since C and O are
thought to be produced only during hydrostatic phases of stellar evolution the
[C/O] versus [O/H] trend in the Galaxy should be considerably simpler to predict
than [C/Fe] and [O/Fe], because iron is produced in the hard to model explosions of Type~Ia
and Type~II SNe in quantities that are not well predicted.  Indeed, even the theoretical
yields for Mg from Type~II SNe (e.g. from WW95) are not well predicted
and it has been necessary for modellers to employ semi-empirical yields
from Galactic chemical evolution models (e.g. Fran\c cois et al. 2004).

In this paper we analyse the effects of stellar yields with mass loss on carbon and
C/O ratios, both in the bulge and the disk.  As mentioned before, the
decreased O production results in an increased C production and this effect needs
to be tested with the observational data. Besides the Maeder (1992) yields,  we have included in the chemical
evolution models C and O yields from massive stars by Meynet \& Maeder (2002),
computed with a lower rate of mass loss but including rotation; yields for Z=0.02
stars, which were not given in the original paper, were taken from Chiappini et al. (2003b).
Yields for super-solar metallicity stars are not available.

The paper is organized as follows: in Section 2 we describe the observational data,
in Section 3 we recall the main assumptions of the adopted chemical evolution models,
in Section 4 we describe the adopted stellar yields, in Section 5 we show the
results for the bulge and the disk of the Milky Way. Finally, in Section 6 some
conclusions are drawn.

\section{Observational data}\label{data}

We wish to compare the observed trends of [C/O] with [O/H]
in the Galactic thin and thick disks and bulge with predictions of chemical evolution
models including yields from stars with metallicity-dependent winds.  For the
relatively hot unevolved turn-off and main sequence stars carbon and oxygen abundances
are most reliably determined from the forbidden [O~I] and [C~I] lines at
6300\AA\ and 8727\AA , respectively, because these lines have negligible non-LTE
abundance corrections.  This is unlike the allowed C~I and O~I transitions with large
predicted non-LTE corrections, the estimated values of which have varied significantly
(e.g. Fabbian et al. 2006, 2009).  The insensitivity of the forbidden lines to non-LTE
effects is partly due to the long lifetimes of the upper levels, which allows collisions
to set the populations to their local thermodynamic values.  However, a cause for care
and concern is that the forbidden [C~I] and [O~I] lines are rather weak in the turnoff
and dwarf stars, with equivalent widths typically in the range 2--12 m\AA .  Also, only
in the last few years it has been appreciated (Allende Prieto et al. 2001) that the [O~I]
line at 6300\AA\ is blended with a Ni~I line; and that the [C~I] feature contains a weak
Fe~I blend (e.g. Bensby \& Feltzing 2006) and lies in the wing of a stronger Si~I line.
We note, in passing, that the largely ignored [O~I] line at 6363\AA\ is much weaker than the line
at 6300\AA\ and often gives discordant results, which we presume is related to the fact
that it lies in the middle of a broad Ca~I auto-ionization feature which
depresses the central [O~I] line depth; most studies fail to take the Ca~I auto-ionization
feature into account, resulting in spurious oxygen abundance results.

In this paper we employ forbidden line carbon and oxygen abundances of thin and thick disk
dwarf/turnoff stars from two main sources: Bensby \& Feltzing (2006) and the corrected
oxygen abundances of Nissen \& Edvardsson (1992) and carbon abundances from Gustafsson
et al. (1999) and Andersson \& Edvardsson (1994).  Nissen (private communication) kindly
supplied the revised oxygen abundances, from the [O~I] 6300\AA\ line, corrected for the
Ni~I blend (which was not a known problem in 1992).  While Nissen did not publish the
corrected oxygen abundance values they do appear in Fig.~9 of Nissen et al. (2002).
We have performed calculations which roughly confirm Nissen's corrections.
In Nissen's private communication to us he also included abundances for two extra, unpublished,
halo stars.

In Fig.~\ref{coohsolardata}
we show literature results of [C/O] versus [O/H] for the solar vicinity, based on
the forbidden [O~I] and [C~I] lines.  The plot shows a clear distinction between the [C/O]
ratios in the thin and thick disks; the thick disk is characterised by lower [C/O] values,
which decrease with metallicity, and seem to link to the low [C/O] ratio seen in the two
halo stars.  The good agreement between the Nissen data and those of Bensby \& Feltzing (2006)
is encouraging.  We note that the population identifications are based on statistical
probability, so a small number of misidentifications are possible.  The differences in [C/O]
versus [O/H] for the thick and thin disks show that it was not possible to make the thick disk
from present day thin disk material (e.g. by dynamical heating of the thin disk), or to make
the lower metallicity thin disk from thick disk material (see also Chiappini 2009 and Chiappini et al. in preparation
for a discussion on the different evolution between the thin and thick disks).
\begin{figure}[ht!]
\begin{center}
\includegraphics[width=0.99\textwidth]{coohsolar.eps}
\caption{[C/O] ratio versus [O/H] for dwarf and turnoff stars in the solar vicinity,
based on forbidden [O~I] and [C~I] lines, which are insensitive to non-LTE effects.
The thin disk stars from corrected Nissen \& Edvardsson (1992), Gustafsson et al. (1999)
and Andersson \& Edvardsson (1994), indicated by black crosses are in good agreement
with the thin disk results of Bensby \& Feltzing (2006, red filled hexagons).
Thick disk stars from Bensby \& Feltzing (2006) are indicated with blue open hexagons;
two thick disk stars from Nissen shown with open black squares are consistent with
the Bensby \& Feltzing (2006) results.  Two halo stars from Nissen (private communication)
are shown as filled black squares.  This plot shows a clear distinction between
the [C/O] ratios in the thin and thick disks: the thick disk [C/O] ratios are
significantly lower than for the thin disk toward lower [O/H].}\label{coohsolardata}
\end{center}
\end{figure}
Of course, carbon and oxygen abundance measurements are also possible for red giant stars.
An advantage is that the [O~I] 6300\AA\ line is stronger in red giants ($\sim$30--70m\AA )
than dwarf/turnoff stars; the 8727\AA\ [C~I] line is also stronger in red giants
(e.g. 11m\AA\ in Arcturus), but it has not been used much in these stars.  A significant
disadvantage posed by the red giants is that stellar evolution effects, during the first
dredge-up phase, cause their atmospheres to be altered from their original CNO composition.
In the first dredge-up the atmospheres are contaminated by material that previously experienced
proton-burning by CN cycle core burning (e.g. Iben 1964, 1967; Becker \& Iben 1979).  Typically,
solar neighborhood red giant atmospheres show $\sim$0.2 dex carbon depletions, but 1 dex depletions
are also found (e.g. Lambert \& Ries 1981).
However, because most of the missing carbon is turned into nitrogen the original carbon abundance can
be estimated from the sum of C$+$N.  This is a useful trick for measuring the primordial carbon
abundance in red giants, and especially important for studying the Galactic bulge C/O trend,
since the bulge dwarfs are too faint for routine high resolution abundance studies\footnote{Recently,
Johnson et al. (2008) have measured C/O in a single lensed bulge dwarf star spectrum, but the oxygen
abundance relied on the highly excited allowed transitions at 7770\AA , which are known to suffer
from non-LTE effects.}; thus, red giant stars provide the main probe to effectively explore the
Galactic bulge C/O trend.

In Fig.~\ref{thindiskdata1}
we show the thin disk [C/O] trend with [O/H]
based on the abundances from dwarf and turnoff stars from Bensby \& Feltzing (2006, red filled
hexagons) and Nissen (private communication, red crosses).
In addition to these results from dwarf and
turnoff thin disk stars we also include [C/O] ratios based on the [(C$+$N)/O] values in the red
giants of Mishenina et al. (2006; black filled squares); to do this we sum the C and N abundances
but we also subtract an estimate of the original N abundance, based on the solar N/Fe ratio, which
amounts to almost 0.10 dex.
Fig.~\ref{thindiskdata1}
shows that the three sources of [C/O] versus [O/H] in the thin disk are
consistent with a single trend, and a small decrease in [C/O], of about 0.2 dex, from [O/H]=0.0
to $-$0.4 dex.
 We note that the Mishenina et al. (2006) red giant data lack points at the low [O/H] end
of the diagram; this probably arises from an absence of carbon abundances
for their metal-poor disk stars, due to non-detection of the C$_2$ molecular lines, which they used
as a carbon abundance indicator.  These molecular C$_2$ lines are relatively weak at solar
metallicity, and decrease rapidly in strength to lower metal content.  In addition to the decrease
in [C/O] at low [O/H] there may be a decrease in [C/O] at the highest metallicity
([O/H] $\ge$$+$0.15 dex), but this conclusion is sensitive to outliers in the plot.
If we use only the current carbon abundances for the Mishenina et al. (2006) red
giants, without the correction for the CN cycle transformation of carbon to nitrogen,
the thin disk red giants are not consistent with the trend established by the two sources
of [C/O] ratios for the thin disk dwarf stars, but instead shows depleted [C/O] values by $\sim$0.2 dex.
We take this difference  as evidence that our practice of combining the C$+$N abundances,
minus the estimated original N, for red giant stars provides sound results, and should give
reliable [C/O] ratios when applied to the Galactic bulge red giants. We note, however, that the [C/O] versus [O/H] trend for thin
disk red giant stars in Melendez et al. (2008, henceforth M08) show larger scatter and a
$<$0.1 dex downward shift compared to the dwarf results of Bensby \& Feltzing (2006).  However, the M08 results for the thick disk
are in good agreement with the Bensby \& Feltzing (2006) values, but with somewhat larger scatter.

\begin{figure}[ht!]
\begin{center}
\includegraphics[width=0.99\textwidth]{thindiskdata1.eps}
\caption{[C/O] versus [O/H] for thin disk dwarf/turnoff stars based on forbidden line abundances,
from Bensby \& Feltzing (2006; red filled hexagons) and corrected Nissen (1992; red crosses).
[C/O] versus [O/H] for thin disk red giant stars are from Mishenina et al. (2006; black
filled squares), but corrected for first dredge-up by adding C$+$N (minus the
original N based on the solar N/Fe ratio) to estimate the primordial carbon abundance.
Note the good agreement between dwarf/turnoff stars, which are unaffected by first dredge-up, and
the red giant [C/O] ratios from C$+$N - Fe.(N/Fe)$_{\odot}$.  }\label{thindiskdata1}
\end{center}
\end{figure}

For the bulge [C/O] data we considered abundance results from Fulbright et al.
(2007), M08, and the oxygen abundances from Zoccali et al. (2006)  with carbon
results for the same stars given in the companion paper by Lecureur et al. (2007).
Results from the small overlapping studies of Cunha \& Smith (2006) and
Ryde et al. (2009) could also be included in the comparisons.  We omit the abundance
results for bulge M giants from Rich \& Origlia (2005) and Rich et al. (2007) since
they did not measure nitrogen abundances, required to estimate the primordial carbon.

McWilliam, Fulbright and Rich (2009, in progress, henceforth MFR09) have recomputed oxygen
abundances, for stars in the FMR07 study.  In their molecular equilibrium calculations
they employed the carbon and nitrogen abundances determined from IR spectra in the
same set of stars by M08 (of the 19 bulge stars in M08 18 were studied by FMR07).
The MFR09 abundances are an improvement over FMR07, in part because the FMR07 oxygen
abundances were computed using approximate C/Fe and N/Fe abundance ratios,
expected for typical red giant stars, rather than measured values.  The revised
MFR09 O/Fe ratios were based on line-by-line differential abundances relative to
the sun, using the [O~I] 6300\AA\ line and five transitions of Fe~II.

The differential method employed by MFR09 removed
the $gf$ values from the calculation of the [O/H] and [Fe/H] abundances.
Furthermore, because formation of the Fe~II lines is similar to the [O~I] lines,
errors in parameters that effect the electron density in the stellar atmospheres
(e.g. gravity and $\alpha$/Fe ratio) have a negligible effect on the
[O/Fe] ratio determined using these lines.  We note that Zoccali et al.
(2006) did not discuss the use of Fe~II lines or appropriate alpha-enhanced
model atmospheres in the determination of their [O/Fe] ratios,  because they
used Fe~I lines for the [O/Fe] ratio.  If so, their [O/Fe] ratios would be
strongly dependent on the gravity, metallicity and $\alpha$/Fe ratios of the input
model atmospheres; indeed, their [C/O] versus [O/H] trend shows a much larger scatter
than the trend found here.  Therefore, we respectfully choose not to employ the
Zoccali et al. (2006) [O/Fe] ratios.
For the [Fe/H] abundances MFR09 retained the FMR07 [Fe/H] values,
which were based on differential Fe~I line abundances relative to the nearby red giant
$\alpha$~Boo, and provide [Fe/H] values with small internal scatter.

We note that the [O/Fe] versus [Fe/H] trend of MFR09 and that of M08
agree very well from $-$0.8$<$[Fe/H]$<$$+$0.5 dex, but below [Fe/H]$\sim$$-$0.8
dex MFR09 [O/Fe] values are larger than M08 by
$\sim$0.1 dex.  It is likely that the two OH lines in the M08 spectra are relatively
weak at these lower metallicities, while the [O~I] lines in FMR07/MFR09 are easily
measured.  Differences between the M08 points and MFR09 values are partly due to the
adopted [Fe/H] abundance;
we do not know the cause of the difference between FMR07/MFR09 and M08
[O/Fe] trends at low metallicity.
Perhaps the reduced strength of the Fe I lines, or the small number of
detected Fe I lines, in the near-IR spectra of the most metal-poor stars
in M08 resulted in less accurate Fe abundances.  We also note that the
that the optical [O~I] lines in FMR07 are insensitive to non-LTE effects,
while OH lines are sensitive to non-LTE, which is more significant for
metal-poor stars. For these reasons we prefer to employ
the [O/Fe] values computed by MFR09 with the M08 [C/Fe] and [N/Fe] ratios.

As mentioned previously, the C$+$N $-$ Fe.(N/Fe)$_{\odot}$ provides a good
estimate of the original carbon abundance in red giant stars that have experienced
first dredge-up of CN processed material.   For the bulge results we employ
[O/Fe] from MFR09 and the [C/Fe] and [N/Fe] abundances from M08 to determine
the primordial [C/O] and we use the MFR09 [O/Fe] with FMR07 [Fe/H] ratios to compute
[O/H].

In Fig.~\ref{diskbulgedata}
we show our adopted bulge trend of primordial [C/O]
versus [O/H], estimated from the measured carbon and nitrogen abundances of
M08 and the MFR09 [O/FeII] ratios, from the FMR07 EWs.  For
the [O/H] values we add the FMR07 [Fe/H] abundances to the robust [O/FeII] ratios
of MFR09.  For comparison, the figure also includes the data for thin and thick
disk stars presented in Fig.~\ref{coohsolardata}.
Fig.~\ref{diskbulgedata}
shows a relatively tight correlation of [C/O]
versus [O/H] in the bulge, with a plateau near [C/O]=$-$0.50 dex for metallicities below
[O/H]$\sim$0, but rising, roughly linearly from [O/H]$\sim$$-$0.1, with increasing
metallicity to [C/O]$\sim$$+$0.1--0.2 dex near [O/H]$\sim$$+$0.3 dex.  The most obvious
feature is that the bulge [C/O] versus [O/H] trend is remarkably similar to that of the
thick disk, and quite different than the thin disk.
We note that the 5 stars from Cunha \& Smith (2006) and the 3 stars from Ryde et al. (2009),
most of which are in FMR07 and M08, show similar [C/O] versus [O/H] to those seen in the bulge
in Fig.~\ref{diskbulgedata}, but with larger scatter than our data.  However, there simply
aren't enough points in either of these two studies for a useful comparison.  Two of the
stars in Ryde et al. (2009) are in Cunha \& Smith (2006), but for one (BW IV-329) their
abundances differ significantly.  In addition, the Ryde et al. (2009) [C/O] and [O/H] values
for BW~IV-203 place it far from the remaining points in Fig.~\ref{diskbulgedata},
 due to it's enormous nitrogen abundance; also,  FMR07 determined that this star
was not a member of the bulge by comparing photometric and ionization based gravities, as stated
in that paper.
Given the
much larger sample of stars in MFR09 and M08, the small scatter evident in the
bulge [C/O] ratios of Fig.~\ref{diskbulgedata},
the use of the forbidden [O~I] line here, and the uncertain systematics of
the Ryde et al. (2009) and Cunha \& Smith (2006) results we, respectfully, prefer not to
use the latter.

\begin{figure}[ht!]
\begin{center}
\includegraphics[width=0.99\textwidth]{diskbulgedata.eps}
\caption{ Our estimated primordial [C/O] versus [O/H] trend in Galactic bulge
red giants (cyan filled hexagons), determined from FMR07, MFR09 and M08, compared
with the thin disk (red filled hexagons and black crosses) and thick disk
(blue open hexagons and black open squares) dwarf/turnoff stars (identical to
Fig.~\ref{coohsolardata}).  The primordial values
for the bulge red giants were estimated from {(C$+$N) $-$ Fe.(N/Fe)$_{\odot}$}.  The tight
correlation of [C/O] versus [O/H] in the bulge appears identical to the relationship
seen in the thick disk stars.  }\label{diskbulgedata}
\end{center}
\end{figure}

\section{The chemical evolution models}

For studying the chemical evolution of the solar neighbourhood, we adopted the model
of Fran\c cois et al. (2004), which is an implemented version of the original model
by Chiappini et al. (2003a). This model assumes that the Galaxy formed by means
of two main accretion episodes, one giving rise to the halo and thick disk and
the other forming the thin disk.
The infalling gas is always assumed to be of primordial composition. Detailed
nucleosynthesis from low and intermediate mass stars, Type Ia and Type II SNe is
taken into account. The IMF is taken from Scalo (1986).  For details of this model
see Fran\c cois et al. (2004).

For the bulge, we adopted the model of Ballero et al. (2007a), which assumes a rapid formation
timescale, of 0.3--0.5 Gyr, from gas accumulated during the Halo collapse.
The efficiency of star formation (star formation per unit mass of gas) is
20 times
higher (i.e. $20 Gyr^{-1}$) than in the solar vicinity ($1 Gyr^{-1}$).
The IMF is flatter than in the solar vicinity, as required by the observed
bulge stellar metallicity distribution:  we assumed the following
IMF: x=0.95 for stars with $m > 1M_{\odot}$, and
x=0.33 for stars with $m \le 1M_{\odot}$ (see Ballero et al. 2007a for details of this model).

\section{Nucleosynthesis Prescriptions}{\label{NP}}

In this work we investigate 3 different prescriptions
for the yields from  massive stars, in particular: i)
the metal dependent yields of Woosley \& Weaver (1995, hereafter
WW95), ii) the metal dependent stellar yields
from massive stars of Meynet \& Maeder (2002, hereafter MM02), which
take into account the effects of mass loss and rotation on stellar evolution,
used also in Chiappini et al. (2003b),
iii) the yields with mass loss and no rotation of M92.
It is worth noting that both the M92 and MM02 yields from massive stars
include mass loss by stellar winds, but the MM02 calculations adopt a
significantly lower rate of mass loss. The recent mass loss rates are factors
of 2 to 3 times lower than previously adopted by M92 and they include stellar
rotation.
\\
For low to intermediate mass stars we use in all the models
the van den Hoek \& Groenewegen (1997) metallicity dependent yields
(in particular the tables assuming a mass loss parameter, $\eta$, varying with metallicity).
We also tested the Karakas \& Lattanzio (2007) metallicity dependent yields of C
and O from low and intermediate mass stars, and found negligible differences in the results
compared to those obtained  with the van den Hoek \& Groenewegen (1997) yields. We then
 adopted the latter ones for consistency with our previous paper (McWilliam et al. 2008).

We note that the more recent oxygen yields of Hirschi et al. (2005) are significantly higher
than MM02, by factors of 2--3.  In fact, Hirschi et al. (2005) stellar evolution calculations
were carried out with different input parameters (e.g. different amounts of  overshooting).
Moreover they only included material lost in the wind, and nucleosynthesis up to the pre-SN stage;
they did not include any treatment of the supernova explosion,
explosive nucleosynthesis calculations (e.g. explosive O burning), or other issues related
to SN nucleosynthesis yields, as discussed in WW95 and many other works.
Therefore, we avoid combining these different set of yields which otherwise
would produce an artificial metallicity dependency of the oxygen yields.

The M92 and MM02 yields did not perform supernova nucleosynthesis calculations, but they
employed the Arnett (1991) relationship between O yield and the M$_{\alpha}$ core mass
to determine their oxygen yields.  The Arnett (1991) O yield relationship with M$_{\alpha}$
is very similar to the independent result of WW95.

For Fe we compute all the models with
the stellar yields by WW95 at solar metallicity for Type~II SNe, which give the
best agreement for the solar vicinity (see Fran\c cois et al. 2004).\\
For the yields from SNe Ia we adopt those of Iwamoto et al. (1999) where
each SN produces 0.6$M_{\odot}$ of Fe.

\section{Results}

We run several models for both the bulge and the solar vicinity with
yields from massive stars taken from various authors:
A) metallicity-dependent WW95 yields, without mass-loss;\quad
B) WW95 yields for metallicities
below solar and the M92 yields (with mass loss) for $Z \ge Z_{\odot}$;\quad
C) WW95 yields for metallicities lower than solar and MM02
yields (including mass-loss) for  $Z \ge Z_{\odot}$;\quad
D) MM02 metal-dependent yields (with mass loss) only.

\begin{figure}[ht!]
\begin{center}
\includegraphics[width=0.99\textwidth]{coohsolartheory.eps}
\caption{Predictions of [C/O] versus [O/H] in the thin disk compared
to measured abundances in the solar vicinity.  See Fig.~\ref{coohsolardata}
for the key to the data symbols.  We present the results of four different
chemical evolution models, with and without metallicity-dependent yields.  To better
match the [C/O] versus [O/H] slope in the bulge (c.f. Fig.~\ref{bulgetheory}) we interpolate
MM02 and M92 yields between Z=0.004 and Z=0.002.}\label{coohsolartheory}
\end{center}
\end{figure}

In Fig.~\ref{coohsolartheory} we show the results of four chemical evolution
models compared with the solar neighborhood [C/H] versus [O/H] trends for the thin and
thick disks.  A strength of this plot is that only C and O are involved, so complications from
the production of Fe in Type~Ia and Type~II supernovae are avoided.  Because carbon and
oxygen are produced during hydrostatic phases of stellar evolution the yields are much more
tractable than for for Fe.

The predictions for the thin disk [C/O] trend show an increase in the [C/O] ratio associated
with carbon production from relatively low mass stars, on long timescales ($>$1Gyr).  This
partly agrees with Bensby \& Feltzing (2009) conclusion, who argued that the production of
carbon occurred on a similar timescale to the production of Fe, based on a flat [C/Fe]=0.0
trend for both the thin and thick Galactic disks below solar [Fe/H].  Our interpretation
based on the data and our predictions in Fig.~\ref{coohsolartheory}
is that the thin disk shows higher [C/O] ratios than the thick disk, due to increased carbon
yields from low mass stars;
our predictions show such increased carbon yields on long time scales (from low mass stars)
for the thin disk only.  Our thin disk models suggest that approximately 50\% of the
carbon produced along the whole galactic history comes from low mass stars.

We presume that, similar to the bulge, the thick disk evolved more rapidly than the thin disk
(see also  Melendez et al. 2008), given the similarity of the thick disk and bulge [C/O] versus
[O/H] trend in Fig.~\ref{diskbulgedata}.
Therefore, the thick disk would not be expected to have included the extra carbon produced
on long time scales by low mass stars; this is in contrast to the conclusion of Bensby \&
Feltzing (2009).

Several features in Fig.~\ref{coohsolartheory} are worthy of note: first,
the slope of the [C/O] versus [O/H] trend in the thin disk is best matched by models C and D,
which employ the MM02 yields with metal-dependent stellar winds plus rotation.  The higher
mass-loss rates used in the M92 metal-dependent winds result in too steep a [C/O] versus [O/H]
slope, as if too much carbon is released at the expense of oxygen.  On the other hand model
A, which employed the metal-dependent evolution of WW95 but ignored mass loss from stellar
winds and rotation, gave too shallow a slope in the [C/O] versus [O/H] relation for the
thin disk.

We draw attention to the inflection points in our thin disk models in Fig.~\ref{coohsolartheory},
where [O/H] appears to decrease temporarily.  This is due to the competition between the star
formation rate (SFR) and the gas infall rate.
In fact, in the two infall model a gap in the SF is naturally produced at the end
of the halo-thick disk formation.  Such a gap is mainly due to the different infall episodes
coupled with a threshold in the gas density for SF (see also a discussion of this point in Chiappini et al. 2003b).
At the inflection
point, star formation is not active because the infalling gas forming the thin disk has still a density below the threshold.
Therefore, O is no more produced while the thin disk is growing by means of H infalling gas.
At later times, on long timescales, the disk [O/H] increases
again, due to the activation of SF and to the diminishing effect of the declining infall rate.
Also, the [C/O] ratio increases further due to carbon from long-lived stars.

The maximum [O/H] and [C/O] ratios reached by our models is also worth noting:
Fig.~\ref{coohsolartheory}
shows a progression in the maximum [O/H] from the models that
decreases with increasing stellar wind mass-loss rate, while the [C/O] ratio increases
with increasing stellar mass-loss rates (WW95$<$MM02$<$M92).  These maximum ratios are
simply due to the increase in carbon yield, at the expense of oxygen, as the mass-loss
prescription is increased.  Clearly, none of our models reaches the highest
[O/H] values observed in the thin disk.  The solution to this lacuna is not obvious:
perhaps the theoretical nucleosynthesis yields need to be increased (e.g. due
to nuclear reaction rates or stellar evolution effects), or we should include in the models the migration
of more metal rich stars in the solar vicinity (see Sch\"onrich \& Binney 2009). Ideally, our predictions should match
both the [C/O] trend with [O/H] and the [O/H] distribution function, similar to the metallicity
distribution function (MDF) from [Fe/H] frequently used to constrain the gas infall rate parameter.

It is encouraging that the thin disk [C/O] observations nicely overlap our predictions, at least
for [O/H] less than solar, but zero-point shifts due to the exact value of the solar oxygen and
carbon abundances could slightly diminish this pleasing agreement; Asplund's group have recently
suggested an increased solar oxygen abundance, by 0.05 dex (Scott et al. 2009).  Other
zero-point shifts may occur if theoretical yields are over/under estimated, or sources omitted;
however, differences between predicted trends between the thin disk and bulge/thick will be more robust.

In Fig.~\ref{bulgetheory}
we show the [C/O] versus [O/H] data and predictions from our
bulge models.  We note that for the models that employ the MM02 and M92 yields we have interpolated
the metallicity-dependent yields between Z=0.02 and Z=0.004.  We believe this to be a reasonable
procedure, but if this interpolation is not adopted then the predicted [C/O] trends rise nearly
vertically, much steeper than the gentle positive slope described by the data; we have employed
this same interpolation of yields over metallicity for the thin disk models previously described.
We first note
that the predictions with the metallicity-dependent yields from WW95 completely fail to
match the bulge observations, while the shape of the observed upward trend in [C/O] with increasing
[O/H] seems to fall between the predictions based on the MM02 and MM92 yields affected by
metallicity-dependent winds in massive stars.  We take these predictions as strong evidence that
yields from massive stars with metallicity-dependent winds are largely responsible for the increase
in observed trend of [C/O] and the decrease in observed trends of [O/Mg] (and [O/Fe]) in the bulge.  Thus,
the apparent inconsistency between the enhanced [Mg/Fe] ratios and declining [O/Fe] with [Fe/H]
in the bulge is simply a metallicity effect, as suggested by McWilliam et al. (2008).
Apparently, the metallicity-dependent winds do not decrease the Mg yields as much as the O yields.
 It is worth noting that
for the thin disk the increase in the [C/O] trend is mainly due to the contribution of intermediate and
low mass stars at low [O/H] because of the low star formation rate in the thin disk, whereas the increase of
[C/O] trend in the bulge is mainly due to the C produced by massive stars occuring at a high [O/H] because of the fast
star formation rate in the bulge. In other words, the different star formation rates in the bulge and thin
disk produce quite different [O/H] - age relationships, with the bulge reaching very fast high [O/H] values.

\begin{figure}[ht!]
\begin{center}
\includegraphics[width=0.99\textwidth]{bulgetheory.eps}
\caption{Model predictions compared to observed [C/O] versus [O/H] in the Galactic bulge.
Model A (red solid line) shows the expected trend for WW95 yields, which did not include
metallicity-dependent mass-loss.  Model B (blue solid line) shows our predictions with
WW95 yields at low metallicity but M92 yields for solar metal content.  The M92 yields include
the effects of metallicity-dependent winds at relatively high mass-loss rate, but did not
include rotational effects.  Model C (green dashed line) shows the result when the lower
mass-loss rates, but including rotation, of MM02 are included, together with the WW95 yields for low metallicity.
Model D (black dotted line) employs
only the MM02 yields which include metallicity-dependent winds and rotation.}\label{bulgetheory}
\end{center}
\end{figure}

Closer inspection of Fig.~\ref{bulgetheory} shows that below [O/H]$\sim$$-$0.2 dex the
[C/O] ratio in the bulge is roughly constant, near $-$0.5 dex.  This differs from the
predicted [C/O] level near $-$0.7 dex.
To explain the difference between the observed and predicted [C/O] ratio in the metal-poor bulge
one might appeal to the bulge IMF slope for massive stars, because more massive stars have lower [C/O]
yield ratios, due to the larger core masses.  However, the bulge IMF slope has been set by
Ballero et al.  (2007a) at x=0.95 in order to explain the combination of a near-solar mean metallicity
distribution function and the high [Mg/Fe] (which suggests a rapid formation timescale).  Thus the
bulge IMF, which Ballero et al. (2007a) require to be skewed to more massive stars than the disk, can
only be significantly altered if the bulge did not form rapidly (contrary to the [Mg/Fe] evidence).
The black horizontal lines marked on Fig.~\ref{bulgetheory}
show the [C/O] ratios for two IMF slopes: x=0.95, the Ballero et al. (2007a) bulge value, and x=1.70,
the Kroupa (2002) value for the solar neighborhood (corrected for binaries).  The masses in
parentheses indicate the lower mass limit of the IMF integrations.
A 9M$_{\odot}$ limit shows the [C/O] ratio produced by Type~II supernovae only, while the
3M$_{\odot}$ limit indicates the lowest mass star that could have died during the bulge formation
time ($<$1Gyr).
Thus, to explain the bulge [C/O] plateau at lower [O/H] would require an IMF slope of
approximately x=1.3.

Other possibilities that could increase the predicted [C/O] in the low metallicity bulge
are: 1.  The C production from very fast rotating extremely metal poor stars, but in this case a plateau in [C/O] would
not be obtained but rather an initial peak followed by  a further decrease (see Chiappini et al. 2006),
although in a starburst situation, such as in ellipticals or bulges, fast stellar rotators
could have been present up to larger metallicities, as recently suggested by Pipino et al. (2009).
2. A decrease in the $^{12}$C($\alpha$,$\gamma$)$^{16}$O rate, although we are unable to
give a quantitative estimate or say whether this can reasonably be the case.  3. An extra
source of carbon at low metallicity could be provided by low metallicity massive binaries.
We recall that an early
suggestion for the production of Wolf-Rayet (WR) stars was through Roche lobe mass-loss/stripping
of the outer envelopes of massive stars (Paczy\'nski 1967).  While this mechanism is not favored as
the main source of WR stars in the Magellanic Clouds and Galaxy, it should have occurred at some
level, even in low metallicity massive binaries.  Given that the stripping of the envelopes of
massive stars by winds at solar metallicities is responsible for the increased carbon and decreased
oxygen yields, it seems possible that metal-poor WR stars formed through Roche-lobe mass loss in
binary systems would also have increased carbon and decreased oxygen yields.  Quantitative
calculations are required to determine whether this mechanism could have produced the observed
[C/O] ratio in metal-poor bulge stars.  We assume that at high metallicity the Roche lobe stripping
of metal-poor massive binary star envelopes is pre-empted by the effects of metallicity-dependent
winds, so this particular extra source of carbon probably mainly affects the metal-poor regime.
\begin{figure}[ht!]
\begin{center}
\includegraphics[width=0.99\textwidth]{OMgMgH.new2.eps}
\caption{ Comparison between the predictions of our 4 models for [O/Mg] vs [Mg/H]
and the observations in the bulge.
The observational data for the bulge are:
the filled circles are the data from MFR09 and FMR07;
the  open triangles are by Lecureur et al. (2007);
the plus signs are  the infrared results from Rich \& Origlia (2005).
Note that the two bulge stars in parenthesis (from FMR07) show the effect of proton
burning products in their atmospheres, therefore, they have probably suffered
a reduction in the envelope oxygen abundances via stellar evolution,
so their oxygen abundances do not reflect the bulge composition. Left panel: the model results are normalized to
Asplund et al. (2005) solar abundances. Right panel: the model results are normalized to the solar abundances
of Grevesse \& Sauval (1998).}\label{omgmgh}
\end{center}
\end{figure}
 Finally, we should take in account that another option to explain the disagreement between
predictions and observations is represented by the uncertainties in the observational data. \\
In Fig.~\ref{omgmgh} we show the [O/Mg] vs. [Mg/H] in the bulge.
This figure is similar to the one in McWilliam et al. (2008) with the addition of the predictions of
models C and D not present in that paper. Another difference with the same figure in
McWilliam et al. (2008) is that here we adopted interpolated yields, as explained before.
This makes the [O/Mg] ratio to decline less abruptly. We note that, apart from a zero
point problem, the best slope for the [O/Mg] ratio for [Mg/H]$>0$ is still obtained
with the M92 yields (model B), but models C and can still be acceptable.
Concerning the zero point, as already discussed in our previous paper, the agreement with observations depends also on
the assumed solar abundances: here we
have normalized all models to the Asplund et al. (2005) abundances. If we had assumed Grevesse \& Sauval (1989) normalization,
as in Ballero et al. (2007a), the predicted [O/Mg] would decrease by $\sim 0.2$ dex, in very good agreement with the data,
as shown in the figure.
A better agreement could be obtained also by adopting
a steeper than Ballero et al. (2007a) IMF for the bulge,
as discussed for Fig.~\ref{bulgetheory}, which would  lower the [O/Mg] ratio by
$\sim$ 0.2 dex. However, a steeper IMF for the bulge would not account for the stellar metallicity distribution nor for
the mean metallicity in the bulge (see Ballero et al. 2007b, Pipino et al. 2008). Finally, part of the problems could reside
in the still uncertain Mg yields.

\section{Discussion and Conclusions}

We have reviewed stellar CNO abundances in the thin and thick disks and the bulge of the
Galaxy.  Because the bulge red giant stars envelopes are contaminated by first dredge-up,
CN processed, material in their envelopes, we estimate the their primordial [C/O] ratios
from C$+$N minus a correction for the original nitrogen abundance ($\sim$0.1 dex).
We showed that with careful measurements this method can give [C/O] ratios from red giants
identical to unmixed dwarf/turnoff stars in the thin and thick disks.

From our review of such CNO abundances in Galactic bulge red giants we find a large
increase in the [C/O] ratio ($>$0.5 dex) that is tightly correlated with metallicity
between [O/H]=$-$0.1 and $+$0.4 dex.  This observed change in bulge [C/O] ratio
can be reproduced with bulge chemical evolution models that incorporate
yields from massive stars including the effects of metallicity-dependent stellar winds
and rotation; in particular our models would best match the observations with mass-loss
rates intermediate between the values adopted by M92 and MM02.  This supports the idea
that the decline in [O/Mg] and [O/Fe] seen in the bulge near solar metallicity is
due a decline in oxygen yields in massive stars by metallicity-dependent winds, as
suggested by McWilliam \& Rich (2004) and McWilliam et al. (2008).  This is important
because it resolves the apparent discrepancy in interpretation of the bulge formation
timescale based on simplistic interpretation of the bulge trends of [Mg/Fe] and [O/Fe].
These conclusions on the bulge [C/O] ratio support a rapid bulge formation timescale ($<$1Gyr).

To better match the slope of the bulge [C/O] ratio with [O/H] we found it necessary to
interpolate the predicted stellar yields, rather than employ a step function change in
yield at solar metallicity.  We employ the same interpolation technique for our models
of the thin disk [C/O] trend with [O/H], and we find a remarkably good correspondence between
our model results and the thin disk observations. In particular, we find that the [C/O]
slope in the thin disk is best matched with the yields of MM02.  In our models approximately
50\% of the thin disk carbon comes from low mass stars.

M08 found that the bulge and thick disk [O/Fe] versus [Fe/H] trends are identical; our
new oxygen results in MFR09 agree with this conclusion.  Remarkably, the data examined here
shows that the [C/O] versus [O/H] locus in the thick disk is also practically identical to the
trend in the Galactic bulge.  We assume that the common trends in these two systems is due to
higher star formation rates, and faster formation timescales, than occurred in the thin
disk.  However, the higher [Mg/Fe] in the bulge than the thick disk (FMR07) is evidence that
the bulge formed more quickly.  Still, while the bulge and thick disk
probably formed fairly rapidly it is remarkable that these two systems have such different mean
metallicities ($\Delta$[Fe/H]$\sim$ 0.5 dex).

 As mentioned earlier, Ballero et al. (2007a,b)
employed a shallow IMF (i.e. more high mass stars) in order to fit the bulge stellar metallicity distribution as well as
the bulge mean metallicity with a rapid formation timescale.  Similarly, it may be that while the thick disk and the bulge
both formed fairly quickly (at least relative to the thin disk),
metallicities may largely reflect different SF efficiencies (lower in the thick disk, Chiappini 2009), and/or different IMFs.
 In other words, our best model for the bulge cannot reproduce the mean metallicity and the metallicity distribution of
the thick disk stars.

While our models naturally explain the increase in the [C/O] ratio to higher metallicity,
there is a plateau at low [O/H] in the bulge data; a similar plateau is also seen in our models,
but $\sim$0.2 dex lower than the observations.  While this plateau problem could, in principle,
be solved with a change in the bulge IMF this would lead to a conflict with the observed mean
metallicity and the rapid bulge formation timescale indicated by [Mg/Fe]; thus, we rejected
appeals to the IMF to solve the problem.  The under-predicted plateau suggests to us that there
is a missing source of carbon in our models, and/or an under-production of oxygen.
 Extremely metal poor stars ($Z \sim 10^{-8}$) can be very fast rotators, suffer heavy mass loss and
produce that extra C (Hirschi 2006, Chiappini \& al. 2006), but to  explain the plateau such a production
should extend also to stars with higher metallicities.
Another cause, although prosaic, can be an incomplete stellar evolution physics, wind physics, or
error in the adopted $^{12}$C($\alpha$,$\gamma$)$^{16}$O rate. We highlight an alternative explanation:
stripping of the envelopes of massive stars in binary systems through Roche lobe overflow, which
would work even at low metallicity where winds don't.  We presume that this form of envelope
stripping would also result in an increase in carbon yield at the expense of oxygen.
 Finally, the disagreement between theory and observations could be ascribed to observational
uncertainties.

\section{Acknowledgments}
G.C. acknowledges financial support from the Fondazione Cassa di Risparmio di Trieste.
G.C., F.M.and C.C. acknowledge financial support from PRIN2007-MUR (Italian Ministry of University and Research).
Prot.2007JJC53X-001.
C.C. acknowledges financial support from the Swiss National Foundation (SNF).
F.M. thanks R.M. Rich for many illuminating discussions.
We thank the referee, Martin Asplund, for his careful reading and his suggestions.

redpajama_set_name: RedPajamaArXiv


text:
Edwardsiana alnicola är en insektsart som först beskrevs av Edwards 1924.  Edwardsiana alnicola ingår i släktet Edwardsiana och familjen dvärgstritar. Arten är reproducerande i Sverige. Inga underarter finns listade i Catalogue of Life.

Källor

Dvärgstritar
alnicola

redpajama_set_name: RedPajamaWikipedia


text:
You are here: Home / American Philanthropy / Drop in Giving Expected in 4th Quarter
Drop in Giving Expected in 4th Quarter
After growing 7.7 percent in the first nine months of 2010, compared to the same period last year, overall contributions to charities and churches are expected to fall to $104.18 [billion] in the final three months of the year, down 1 percent compared to the same period last year, according to a new forecast.
The decline is expected because of consumer mindsets, persistently high unemployment, a slowdown in the economic recovery, and the anticipation of big increases in individual federal tax rates that will take effect Jan. 1, 2011, says Philanthromax in its inaugural The Atlas of Giving forecast.
"The timing of the decline is significant," Rob Mitchell, CEO of Philanthromax, says in a statement. "For many charities, fourth-quarter income is the difference between a good and a bad year."
The decline in giving will be greatest in November and December, when gift totals are expected to fall 3.1 percent, compared to the same period in 2009.
"The best thing nonprofits can do right now is to get fundraising appeals out early," Mitchell says. "The later into the year they wait, the more negatively their results will be impacted."
Reprinted with permission of Philanthropy Journal.
Filed Under: American Philanthropy, In the Media


People keep telling me how weak Tetsuko is.
Then they sulk (and/or cry).
Welcome to my most oppressive deck!
Story time! When I first learned Magic, back in 2003, I only had one friend to play against, who had more money and experience than me.
Using a vicious mono-blue control deck, he brutally defeated me every day...for four years. When I finally beat him, he literally burned his cards and quit the game rather than play against me again. I was left with nothing, except a visceral hatred for blue mages.
When playing this deck, I want to share this experience with my opponents.
...Okay, I'll admit it, it turns out that I'm a bit of a control freak. You either die a hero, or live to see yourself become the villain, as they say.
This is a mono-blue control/aggro list. It's optimized for 1v1 play (where your counterspells do the most work), although it still definitely works in multiplayer. The deck is built around combat damage triggers, particularly ones that draw cards or disrupt opponents. The goal is to slowly whittle down our opponents' hand and resources, counter whatever wincons they try play, and beat them to death with our army of tiny blue beaters.
The goal is to control at least a few creatures that draw cards upon connecting with opponents, so that you draw 4+ cards per turn, and use this card draw to dig for answers and counterspells.
In order to win in a reasonable amount of time, we have several methods to boost creatures' power while still leaving them unblockable ( Umezawa's Jitte , Runechanter's Pike , etc), use infect ( Inkmoth Nexus ), use Quietus Spike , or create our own pseudo-Annihilator ( Cephalid Constable ). When playing this deck according to the 1v1 banlist, the deck adds a few other "fast" win-cons as well. Don't forget that 6/1 creatures are still unblockable due to Tetsuko's ability, but 6/2s are not.
This deck gets most of its card advantage from having its creatures connect with opponents, often with the help of Tetsuko's ability. We are running 6 creatures that automatically draw a card when they hit an opponent, in addition to 4 non-creature spells that have similar effects ( Bident of Thassa , Coastal Piracy , Smuggler's Copter , and Mask of Memory ) - in effect, we are running 10 copies of Phyrexian Arena in the deck. As long as we control 1 of these creatures, we rarely run out of cards to keep up with our opponents. On a good hand, such as Master of Waves accompanied by Tetsuko and Bident of Thassa , we can easily be drawing 7+ cards per turn.
Other non-draw combat triggers are covered in the sections below, but they generally have some form of disruptive effect to our opponents' plans.
Preemptive disruption can be anything from stax pieces (such as Damping Sphere or Arcane Laboratory ) to silver-bullet answers ( Phyrexian Revoker ), to hand disruption ( Riptide Pilferer or Vendilion Clique ) to library-attacking spells (Riptide Thief or Raven Guild Master ). I will go into further detail later in this primer, but your suite of preemptive disruption can be tailored to your meta and opponents if you know their deck well. Our final form of preemptive disruption is to attack landbases, through cards like Strip Mine , Wasteland , Back to Basics , or often a Stifle pointed at an early fetch land (or under rare circumstances, Commandeer ing an early mana rock).
Long story short, we have many ways to neuter opponents' threats before they even have the chance to try and cast them.
This deck runs 11 pure counterspells, of which 6 are truly unconditional. It also runs Stifle and Nimble Obstructionist as pseudo-counterspells to answer battlefield-based effects such as Aetherflux Reservoir or several infinite loops, as well as interfering with fetch lands. Beyond these counterspells, we also have access to Commandeer , which can be amazing 0-mana disruption against non-creature win-cons, such as powerful planeswalkers or enchantments.
Most of our battlefield disruption is based on bounce effects - making our opponent cast each permanent 5 times forces them to waste mana, and gives us many more opportunities to counter them. Cephalid Constable , Mistblade Shinobi , Sigil of Sleep , and Arm with AEther can bounce opposing threats upon combat.
Meanwhile, we have mass bounce effects from Cyclonic Rift , Thing in the Ice Flip, Crush of Tentacles , and Wash Out , in addition to repeatable targeted bounce from Capsize and "bounce" effects from AEtherspouts . Overall, bounce effects are the bread and butter of our temporary removal. When playing in 1v1, I would swap River's Rebuke over Crush of Tentacles , by the way.
Finally, Curse of the Swine , Reality Shift , Rapid Hybridization , and Pongify are valuable because they are some of the very little perma-removal that blue has access to. I would generally save these for when you are desperate or you think that your opponent has no other threats, since they're too important to waste on something smaller.
And, of course, I win more than half my games from concession at this point. Once this deck gets rolling, it's more oppressive than you can possibly believe.
Overall, the plan for this deck is to stall, then win in the late-game once your opponents' threats are neutralized, countered, or disabled. This is in fact harder than it sounds, because this deck has very little at the high end of its curve - you will almost always be winning with 2-4 drops. However, you'll find that you can frequently answer everything your opponents throw at you, and simply win once they've started top-decking.
Against an aggro deck, Propaganda , Mistblade Shinobi , and Cephalid Constable are your best options. Continually bouncing an opponent's creatures before they can hit you is a completely viable way to stall games. Since aggro decks generally run out of steam in the late-game, your goal is to shut down their early pushes (with cheap removal/counters, Curse of the Swine , etc), and overpower them with card advantage and answers in the late game. It's not uncommon to fall below 15 life before stabilizing in this matchup.
Against combo decks, your best answers are generally Arcane Laboratory , Damping Sphere , and a good knowledge of what they plan to do. As everyone knows, combo decks are vulnerable to counterspells, so you have a natural advantage in this matchup. As far as "silver bullets" go, you'll have to decide for your own meta, but I included more information in the "Sideboarding" tab. Don't forget that, if Arcane Laboratory is out, you only need 1 counterspell per opponent to lock them out of casting spells entirely.
Against other control decks, the advice isn't as obvious. They generally play more colors than us, and have more options. I would prioritize countering their board wipes and card draw - since our creatures can draw us several cards per turn consistently, we'll usually outvalue them eventually as long as we protect our creatures on the ground. Reserve your counterspells for things that REALLY need to be answered, and try to play cautiously. Longer games are your friends here.
When playing against multicolored decks, particularly ones with "greedy" manabases, one of your most important cards is Back to Basics . Seriously, the card frequently wins games single-handed against 3+ colored decks. I would personally suggest casting it around T5-6 when they've emptied their hand of lands and tapped out for something.
For the fastest cEDH metas, I would play cards like Spell Pierce and Flusterstorm over some of the more mana-intensive counterspells (such as Cryptic Command or Forbid ). A counterspell doesn't do anything if you don't have the mana to cast it in early turns.
This iteration of the deck doesn't attack opponents' mana as much as some of the earlier drafts: I used to play a solid suite of mana denial ( Winter Orb , Static Orb , Mana Vortex , Land Equilibrium , etc) and ways to get around it ( As Foretold and a few others). If your meta relies more heavily on mana dorks or artifact ramp, you can include Cursed Totem or Null Rod respectively, especially since we are minimally affected by either.
One hard choice when building this deck is choosing which "silver bullet" stax pieces to use. My meta is pretty storm-heavy, so I chose to play the hardest available answers to that strategy ( Arcane Laboratory and Damping Sphere ), but your choices may vary. If you play against reanimator frequently, Grafdigger's Cage might be your best bet; if you play against decks with many ETB effects, Torpor Orb is your friend (especially since we frequently bounce opponents' creatures). If you play against superfriends, Sorcerous Spyglass / Pithing Needle can take their place alongside Phyrexian Revoker . Et cetera - half of the battle in a control deck is knowing exactly what you need to do to shut your opponents down preemptively.
Finally, when playing in 1v1 matches, there are a few changes I would suggest. I would swap in Disallow , Declaration of Naught , River's Rebuke , Island , and Loxodon Warhammer over Back to Basics , Strip Mine , Crush of Tentacles , Mana Drain , and Sol Ring .
...if you savor the salty tears of your opponents like exquisite wine!


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