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IN THE INTERIM: Hudson to coach USMNT in southern California friendlies
Jan 4, 2023 | Men's National Team |
U.S. Soccer sporting director Earnie Stewart Wednesday announced that Anthony Hudson will serve as head coach of the U.S. men's national team for its January training camp in Carson, Calif.
With the ongoing investigation and U.S. Soccer's full review of the USMNT program and head coach Gregg Berhalter following the conclusion of World Cup still underway, Hudson will be joined in Los Angeles by fellow World Cup assistant coach B.J. Callaghan and Under-20 men's youth national team head coach Mikey Varas in selecting and managing the roster for the friendlies against Serbia and Colombia.
Berhalter's contract expired on Dec. 31.
In the past, the customary review of the past four years of the entire program following a World Cup would begin in the summer, well ahead of any year-end contract expiration, U.S. Soccer said in a press release. The unique November-December timing of Qatar World Cup significantly reduced the amount of time that the federation would have to conduct a proper assessment prior to the end of the head coach's contract.
The men will kick off the World Cup 2026 cycle with two matches in Southern California, facing Serbia on Wednesday, Jan. 25 at Banc of California Stadium in Los Angeles and Colombia on Saturday, Jan. 28 at Dignity Health Sports Park in Carson, Calif.
Warner Bros. Discovery Sports will present the games, with specific distribution plans and kickoff times to be announced at a later date.
The two matches will be the first in the four-year run up to hosting the world's biggest sporting event — the 2026 World Cup – alongside Canada and Mexico.
PreviousHE'LL BE RIGHT BACK: NYCFC signs 18-year-old Slovenian defender
NextTHE PLOT SICKENS: Report: Danielle Reyna admits she told U.S. Soccer about Berhalter violence incident
Front Row Soccer editor Michael Lewis has covered 13 World Cups (eight men, five women), seven Olympics and 25 MLS Cups. He has written about New York City FC, New York Cosmos, the New York Red Bulls and both U.S. national teams for Newsday and has penned a soccer history column for the Guardian.com. Lewis, who has been honored by the Press Club of Long Island and National Soccer Coaches Association of America, is the former editor of BigAppleSoccer.com. He has written seven books about the beautiful game and has published ALIVE AND KICKING The incredible but true story of the Rochester Lancers. It is available at Amazon.com at https://tinyurl.com/nfhdk4e5.
OFFSIDE REMARKS: Some Rose Bowl memories of another type of football
FINALLY: Brooks reportedly will sign with Mallorca
THE KIDS ARE ALL RIGHT, BUT …: Sarachan: U.S. youngsters took encouraging 1st steps, but they have a long way to go
WHAT A TV DOUBLEHEADER!: Adams vs. Pulisic in Game 1, U.S. women vs. France in Game 2

redpajama_set_name: RedPajamaCommonCrawl


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all those things are available ftp except for revan and he's been out long enough that when the event returns he's ftp. If you don't have them that's on you.
And making it where new toys won't give an advantage will discourage people from buying said toys. So your idea is not going to happen.
Yeah it does not have to go that far just the ship GP check when no ships
If i have 2 mil toon GP and so does my opponent and he bas 30 more g12 and all the shiny stuff then hey he earned it i can live with it...
If he gets 10 -15 extra teams because of the 400-800k difference in ships thats bad... because we never should have been matched in the first place...
I dont get why its hard to understand for some.... 2 mil vs 2 mil toon gp whatever happens happens
1.8 mil gp vs 2.4 gp toon because ships imbalance he should have been matched elsewhere
How exactly is TW better? You can just as easily face guilds with 2-3x as many Revans as your guild has in TW.
People with Revan aren't being matched with people of lower GP, they are being matched with people who have the same GP but have geared some other character(s) instead of Revan. So I don't understand that part of your point at all.
Not all zetas are created equal, that's true. So the guy in my grouping who decided to zeta Lumi (and is running her under CLS lead in arena!!) should be matched with other people who made similarly silly decisions? Why?
I understand that you are also upset about the "fluff" issue, but you really have to separate the two questions. Whether GP adequately measures the value of g8 vs g12 is a different issue from whether the matching should take into account the differences in characters. If two people have the same number of g12 characters but one person chose to gear the best characters in the game and the other chose to gear random characters he happens to like, the second person should expect to face and lose to the first because that's what happens in a competitive game mode when you choose not to make competitive decisions.
I'm ok with the 3.2 mil vs 3.2 mil total gp and what ever happens happens.
If you have that large of a mismatch because of ships that's likely either rare because your opponent did no ships or you put too much into ships.
Now if they decide to exclude ship gp, that's fine but I don't think it makes the matchmaking inherently unfair any more than letting those with revan be matched with those tgat do not.
Like I said - my bad. I was operating under the assumption that GA was meant to be a fun and competitive game mode for like-rostered players. Apparently you favor the "hand out more gear/rewards to players who paid for X, Y and Z" in every game mode and event. That's fine. Agree to disagree.
I thought players that had Revan were already benefiting enough in arena, TW and HSith raids. Apparently CG (and players like you) feel they should be rewarded even more.
Eventually though, as the game becomes less and less f2p-friendly, the game will cease to exist completely. Whales don't like fighting whales - they like stomping f2p. I get it. Some of my best friends (and those defending this model) are whales. But it's a symbiotic relationship and CG needs to do a better job of maintaining the balance. F2p can't play without whales to pay - but whales won't pay if the guppies all swim to other games either.
Dagobond
I agree. Matchmaking for this mode is terrible. Using GP as a basis ignores many serious differences that have a tremendous impact on a player's ability to compete.
Several of the serious problems with the current matchmaking include:
1) Matching players who don't have a current broken meta, like Revan, against those who do is a sure-fire way to anger a segment of the player base.
2) Secondary speed on mods, which are arguably still the most important determinant of success in fights, are not factored into the matchmaking process at all. Which is incredibly unfair as no amount of money can ensure one will roll decent secondary speed traits.
3) Gear 12, which adds a huge amount of combat potential to characters, seems to have very little influence on GP compared to many other factors.
These are just 3 of the main reasons that CG's matchmaking system is unfair and plain not fun for most players. My guild has already had quite a few people quit the game for a couple of reasons. One reason being the sheer ridiculous amount of time the game now demands with the addition of grand arena (a mode which no one I have encountered likes or asked to see). The other reason many have quit is that the game feels more like being bullied with the current matchmaking fiasco and no one wants to feel that sort of anger in their entertainment.
BanachSpach
I think Grand Arena is one of the greatest additions to the game. I am F2P and I enjoy the challenge of going against stronger opponents. My current opponent had 40 g12 characters to my 19 and I wiped his board. He only cleared one of my territories. He had a better roster, but I had a better strategy, so I won. GA would be boring if I always had the better roster. I like the matchmaking as is.
Rath_Tarr
From my bracket in the first 3v3, no fleet GA...
At approximately 1.5 mill, the Total GP spread used for matchmaking was 1,500 GP (0.001%) but without fleet zones the actual usable GP spread was up to 223k GP (32%)
% squad GP difference for the 56 potential matches in my bracket:
> 30%: 2
25-30%: 4
15-20%: 14
5-10%: 14
< 5%: 10
So 32 of 56 potential matchups gave one player at least a 10% advantage in usable GP or around 150,000 GP worth of toons.
Mzee
3v3 is stupid and needs to stop. Game is designed for 5v5, not for 3v3. Every other game mode since inception has been 5 v 5, NOT 3v3. After winning 1, and then losing another I quit this dumb game mode today.
BanachSpach wrote: »
One of the grand arena main features when it was implemented were "fair" and cool matchmaking and everybody is going have fun. They've somewhat boasted like how good the matachmaking is going to be.
It is great when your opponent sucks. But when going against someone who is a bit conscious about the game and sets up decent defense, having 300k less in character GP is just game over, no matter the strategy.
Players who are invested in the ships a bit more are still at a bit of disadvantage, even when there is a ship territory, but it is still possible to get results. I managed to get to 1st and 2nd places in last 5v5 GAs having less character GP and going against Trayas and Revans while having neither. And I've been 7th on previous 3v3, thought it was my mistakes and didn't bother, it is 3v3 again and I am getting screwed hard, so I've decided to dig a bit, all of my current opponents have 85k to 300k more character GP which translates to a lot more decently geared characters. Yes, we have the same total GP, because I am more invested into ships, but during this 3v3 I can shove all of my ships roster up my a
Why do you have to ruin a great game mode with a stupid 3v3? Why do you have to ruin a great TW game mode with banning a ton of characters, and adding ridiculous bonuses so Ewoks take like 20 teams to take down? My guild won, but it is still annoying. You didn't learn from the invincible Mace Windu gimmick? I like mixing things up, but you always take great game modes and find a way to screw it up. Character, and faction bonuses are a neat idea, but you frequently make them so overpowered that it just isn't fun.
Dagobond wrote: »
Agreed. The matchmaking is broken. GP so far seems to be the best way to match players, but it is still very inaccurate. I don't have Revan, yet I have 4 people in my segment with him, and I find that very irritating. (I am also boycotting this 3v3 from now on and not bothering to set defenses since I hate 3v3)
The matchmaking punishes players who have filled out their roster, which is contradictory to how they have been encouraging players for the last few years. If you gear up lesser characters to boost the GP for Territory Battles like many have then you are at a severe disadvantage. Players who leave all the lesser characters at level 1, and only gear up their main teams are at a heavy advantage. Removing all the mods of lesser characters would help, but what a waste of credits and seems counter-intuitive.
Ships aren't even used in this particular grand arena, but it still counts towards GP, which is silly. I regret leveling up all my pilots and modding them now as it inflates my GP, and I don't want to have to waste credits to remove all the mods, and I wish I left all my useless pilots at level 1 now.
Mods are hidden GP, and makes a huge difference, but I don't have as much issue with matchmaking ignoring this, but perhaps an algorithm could be used to take it into account.
It is an excellent game mode, but from what I have observed after the first time the community overwhelmingly hated 3v3, yet they keep doing it. I don't get it...
Mzee wrote: »
Most teams are built on a foundation of 3 toons. Once you figure out how they function in the 3v3 setting, you can even take our full 5 toon teams with only 3 toons. Bast, Yoda, and a tank. Jango, Boba, cad. The triumvirate. Ventress, Daka, zombie. Cls, han, chewie. There's so many examples of 3 key toons, and two replaceable. Why not do 3v3?
Sewpot
GP should not be the deciding factor for GA. It should matching from 6dot mods and zeta's. Thats a better way to make matches way more even.
Because teams like JTR that are used as a solid counter to Bastille do not work in 3v3. Some teams do work in a 3v3 mode, but many do not.
EDIT: Give me a sec to remove the names
From the current GA; There are only two people with Revan, Mol and UltraZero, and I didn't face him at all. The other three people with 1 win each don't have JKR
Yep, they work, but it doesn't matter when opponents have from 5 to 15 more decently geared up characters, because you are more invested into ships. Very fun to play. You either run out of geared toons or one mistake and you are never going to get enough points. So much fun...
Jtr is a terrible counter for bastilla, even 5v5. Basty will wipe them out under ai 9/10 times.
But my point stands, the choir of that team is jtr, bb8 and r2 usually. It works the same against 3v3 teams as 5v5, as long as it's a good counter to begin with
You can compete ftp. I take top spots in both arenas and all raids and haven't spent a cent.
But I disagree with your premise. Part of the fun of the game is building a roster and seeing how it compares with others. If you matchmake to the point of facing identical rosters, then that removes any incentive to improve your roster.
Rath_Tarr wrote: »
ok and a 10% difference doesn't mean anything. That could be 10% more useless fluff. And even if it's not, it's not insurmountable. The fact that they are using a single factor instead of 10 or 12 factors in matchmaking means that they don't desire perfect matching. But matchmaking that is somewhat close but encourages you to build your roster to do better long-term.
Topcatv2
In the event of a draw, the player with the higher GP wins
Please explain to me how dark ronin gets the win yet it is clearly a draw ?
Higher gp should have no standing on final outcome
Topcatv2 wrote: »
Should've tried to put up a fight then
If i had time to waste, sure... why not... ga, tw, tb are boring... cg come up with something that is actually engaging
Hey i have an idea... battles are not offense defense... it is both... how bout you allow the teams we choose to do both instead of sitting em on the bench?
>I don't want to play or do anything but I want devs to make sure I win
No ultra, that is not the point... it should never be gp based at all... if neither players did attack and placed the same number of teams... it is a draw... size of teams maybe but nowhere is that been mentioned as part of their calculations for ga... so my question is valid... it is a clear draw... zero attempts to attack from either player...
But tbh these events are seriously not engaging... if you want us to spend time playing find a way to allow us to score points on both offense and defense with a single team... no battle is ever like an nfl football game... the only sport in the world that has separate teams...


If you are reading this post, odds are you are savvy with several social media platforms and know how to post on Facebook, write a Tweet, post a pin, upload a few photos, share some links, re-tweet, post onto YouTube and are connected with your business colleagues through LinkedIn and Google +.
Odds are you are also extremely busy, and time is a precious commodity for you, and you know that you likely need to spend more time on your social media strategies to better analyze the social media platforms that you are using.
Firstly, be sure to download a campaign management program such as www.campaignmonitor.com whereby you can set-up and design some great blogs, e-books, and/or a strong email marketing ad campaign. The beauty and ease of these programs is that you can share them across multiple platforms and social media applications such as Facebook, Delicious, LinkedIn, Google Plus, Pinterest, Redditt and Stumble Upon with a simple click.
But before you do this be sure to do some homework with Google Ad Words, so that you can increase your SEO and also do some investigating on the products and/or topics that you are writing about. Again the purpose here is to apply your social media strategies to you blog, your web pages, your e-books, and e-campaigns. It is really important to look for Google Ad Words that have a strong searchable rankings and will optimize your campaign and overall website ranking so that you are climbing the SEO ladder! Again there are many programs out there to analyze your website url performance, and Alexa is a great tool for starters!
Be sure to take 20 minutes to acquaint yourself with Google Analytics and set this up for your company website. Install the tracking code and set some goals for your marketing team to review in a weekly and monthly basis. Again, this will help you set some base lines, and be able to measure the effectiveness of your social media strategies and campaigns. Facebook has a great tool called Page Insights that will give you important metrics on your social media community and how engaged they are with your brand.
Another great blogging and web design program is Word Press, as it is helps you map out your blog or web pages with post titles, meta descriptions, robots Meta configurations – an experienced web designer can help you go through all of this but it is vital that these configurations are done properly to optimize your website ranking. Yoast offers more insight into your blogs and web pages and really is the litmus test for you!
Strategy…Strategy…Strategy! The most important thing we want you to take home with you today for your marketing team is to make sure you have a Social Media Strategy as a complement to your Annual Marketing & Communications Plan. Be disciplined, measure everything and make sure you take time to learn the latest technology out there to keep your brand alive!
Because the web is now the new and powerful "word of mouth" knowing how to leverage its many social media aspects to reach and influence the target audiences groups & discussions where your prospects "hang out" is critical for growing business.
Its also how, without any competition, you become the "go to guru" in the right target audiences, get called and acquire paying customers via the web.
• Where is my target audience? Who are they? Where do they "hang out" online?
• How do they source?
• Where do they go for industry updates and information and how do you get featured "there"?
• How do I think from the point of view of my target audiences so I can relate and connect?
• How do I differentiate myself from the pack so i get called?
• How does my target audience evaluate issues and solutions?
• How can I define my key audiences and position to be of service to each audience so they want what I offer?
• How do I become a featured speaker at events and establish my position as a go to expert?
That reveals where target audiences are, where their "influencers" are and where you should be active via articles, social media, blogs, email, newsletters to create a "go to" national presence and reputation.
* Axiom #1: People do things for their reasons, not yours.
These two principles guide the selling process, whether in letters, emails, your web page, blog or in person. If you remember these two axioms, your sales reach outs and what you say in them will come out as grabbers and connectors with issues and concerns that prospects interested buyers have, not as product pitches and then link/position what you "offer" as a way to solve those issues.
Understanding this thinking in target markets and constructing your reach outs based on the 2 sales axioms can get you the desired national presence and reach that you want plus the all important interested "real" prospect that you want.


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China / Opinion / WHO
Time for China and the WHO to Fess Up
by Professor John West · 28th April 2020
W.H.O. Director-General Tedros Adhanom with chinese President Xi Jinping/ Image: The Atlantic
The Australian government's proposal for an independent international enquiry on the COVID 19 crisis is a much-needed constructive initiative.
The COVID 19 crisis is the greatest disaster and blunder the world has seen since the Second World War.
It is therefore high time for China and the World Health Organization (WHO) to fess up, to be transparent and to ensure that it does not happen again.
Australia's constructive truth initiative
The Australian government's proposal for an independent international enquiry on the origin and handling of the COVID 19 crisis, including the role of the WHO, is a much-needed constructive initiative.
The COVID 19 crisis has highlighted the bankruptcy of China's authoritarian governance which not only greatly facilitates cover-ups and fake narratives, but in that process evidently puts the health of the world's population at risk.
China's swift switch from systems failure to propaganda
China's management of COVID 19 started with a domestic coverup and manipulation of the WHO.
For example, China refused the visit of WHO experts until WHO Director-General Tedros Adhanom met with President Xi Jinping at the end of January, even though the virus was already spinning out of control.
China then progressed very quickly to bumbling attempts at touting the superiority of its authoritarian system.
Some of those attempts at soft power have flopped as China has sold masks and COVID 19 test kits of poor quality, reinforcing an old stereotype China has laboured hard to shed.
A man fixes the chinese flag in front of boxes with Protective suits and masks in Vienna, Austria, Friday, March 20, 2020/ Image: AP Photo/Ronald Zak
Wobbly Chinese soft power diplomacy
Few advanced countries have fallen for Chinese soft power diplomacy. U.S. President Donald Trump has said that China should be punished if it was "knowingly responsible" for the COVID 19 crisis.
British Foreign Secretary Dominic Raab, deputizing for Prime Minister Boris Johnson, said China will have to answer hard questions on how the coronavirus outbreak happened and on whether it could have been prevented.
French President Emmanuel Macron told the Financial Times it would be "naive" to think China had handled the pandemic well, adding: "There are clearly things that have happened that we don't know about."
Poorer countries which depend on Chinese largesse may, however, find themselves more beholden to China, as Beijing seeks to create some strategic advantage from the COVID 19 disaster.
W.H.O. Chief Tedros Adhanom/ Image: The Economist
The WHO's failures
The WHO has not crowned itself in glory either. The COVID 19 episode stands in sharp contrast to the WHO's good work on other pandemics like Ebola, and also in the Pacific.
Of course, like all international organizations, the WHO is vulnerable to pressure from member countries.
But to preserve its credibility, any international organization must stand up unfailingly to protect its core mandate. Its entire credibility rests upon it. In this case, the WHO has been unacceptably subservient to China.
In January and most of February, the WHO wasted precious time as it parroted lines from Beijing. Indeed, the Australian government felt so moved that on February 1, 2020, it defied WHO advice as it implemented a ban on travellers from China.
Two days later, WHO Director-General Tedros Adhanom Ghebreyesus hit out at Australia for the travel restrictions it had issued.
That is not the action of a top manager of global health. That is clearly a case of doing a specific nation's business. Health managers have a clear responsibility to act upon the precautionary principle.
Pandemic management vs. Chinese ideology
Perhaps the most egregious of the WHO's anomalies is the exclusion, because of Chinese political pressure, of Taiwan from the WHO.
Especially because Taiwan has been one of the world's most successful countries in managing the COVID 19 crisis, its exclusion is unacceptable.
U.S. President Donald Trump during Press Conference at White House
Donald Trump vs. the WHO
U.S. President Donald Trump provoked a storm of criticism when he recently announced that U.S. funding for the WHO would be put on hold for 60 to 90 days, pending a review of the WHO's warnings about the coronavirus and China.
While Trump has every reason to question the WHO, his venom towards the organization is widely considered to be a Trumpian ploy to divert attention from his own incompetence.
The reality is that the WHO, warts and all, is a very necessary international organization. It has done much good work in the past. If anything, looking ahead its role needs to be strengthened.
What if the U.S. leaves the WHO?
If the United States were to withdraw from the WHO, that would make the current WHO governance problem only that much worse. It would leave a big gap which China could fill.
That would provide it with yet more space to make the management of global health subject to the ideological whims of the Chinese Communist Party.
And Mr Trump, true to fashion, would have scored yet another own goal, even though his sense that something untoward happened at the WHO is right on target.
That is why the suggestion by the Australian government for an independent international enquiry on the origin and handling of the COVID 19 crisis, including the role of the WHO, is clearly the best way forward.
In today's world, we need middle powers like Australia to step up to the plate and inject some good sense into the international system.
In the meantime, the WHO Director-General would do the organization a favour by resigning immediately from his position and allowing a more credible figure to take over.
This article was originally written for The Globalist
Tags: ChinaTedrosTrump
Professor John West
Professor John West is the author of the recent book, "Asian Century … on a Knife-edge," and executive director of the Asian Century Institute. He is also an adjunct professor at Tokyo's Sophia University where he teaches Japanese Business and Economy and Asia's Economic Development. He can be reached at john.mangwest@gmail.com
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Woman battling brain tumour will see her bucket list dream come true with help from colleagues in Stretford Mall
By Jessica Marsh Reporter
AN inspirational woman battling a brain tumour is to get help making her bucket list of dreams come true, thanks to her colleagues at Peacocks in Stretford Mall.
Just before Christmas, only months after her mum's recovery from breast cancer, Sarah Alouise Cahill was diagnosed with a glioblastoma tumour leaving her, her friends, family and colleagues devastated.
Now, whilst Sarah, 27, undergoes intensive chemotherapy and radiotherapy treatment, her work mates at the Peacocks fashion store in Stretford Mall, are determined to raise enough to send her on the trip of a lifetime.
The team are planning a series of fundraising events to raise £3,000 to send Sarah on her dream holiday to Amsterdam.
The idea came about after shop assistant Sarah drew up her bucket list with her best friend Joanna Walsh, who is assistant manager at the store, and whose eight year-old daughter Brooke Bowden, is Sarah's god-daughter.
Sarah said: "I've never had a 'bucket list', but when the girls at work had the idea to fundraise they asked me to write down some things I'd love to do."
So far, the list has 37 items including, getting matching tattoos, a visit to the "blue roof" at Chillfactor, a spa day, to take a selfie every day, and lunch in a posh restaurant.
She also has a goal to go on a Harry Potter tour for Brooke's ninth birthday, and longer term hopes she will be able to see Brooke make it to high school.
She has even added 'feed a homeless person' to the list, and wants to complete the Race for Life, in aid of the Christie Hospital in Withington, where she is being treated.
Sarah's brain tumour was diagnosed after she collapsed following a prolonged headache – the tumour is stage 4 cancerous and can't be operated on at the moment.
In December 2017, Sarah had surgery to remove some of the tumour but is now pinning her hopes on chemotherapy to reduce the size of the tumour, before another scan in March to decide if more surgery is possible.
Sarah said: "It's a long haul, with no guarantees of recovery.
"At the moment they can't operate but surgery has not been completely ruled out in the future. It depends how successful the chemo is. I'm just trying my hardest to stay positive."
It is the second time Sarah's family has suffered the torment of having to confront the disease after her mum, Carole, battled breast cancer and is now in remission.
Sarah said: "We've had a tough few years as a family, it's been an emotional rollercoaster. Mum was so brave and never gave up. She's really inspired me to fight this thing as courageously as I can."
Twenty-six Peacocks stores across Greater Manchester will fundraise for Sarah's cause across March.
Stretford Mall Peacocks store manager, Mandy Cocker said: "Sarah is hugely popular - we're heartbroken to think of her having to go through this. We're determined to let her know we're all here for her and we've put together an action plan to achieve one of her long held dreams."
Anything Peacocks raise above £3,000 will be donated to The Christie Hospital in Withington that treats more than 44,000 cancer patients a year.
Sarah said: "It really needs the money, the hospital is stretched to the brim, it sees so many patients and the staff work so hard. The hospital desperately needs as much help as we can give it to beat Cancer."
The charity walk will be held on March 18 from Manchester City Centre to Stretford.
To make a donation to Sarah's bucket list fund pop into Peacocks at Stretford Mall.
To join in the Peacocks fundraising walk contact Mandy Cocker or Joanna Walsh at Peacocks, Stretford Mall shopping Centre on 0161 864 1025.
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Every now and then, I challenge myself to eat foods I do not enjoy. Mushrooms, for example. As a restaurant critic, I have now eaten the warm mushroom salad at Hawk's Tavern twice, the first time as a personal challenge, the second because I liked it so much the first time around (and they kept in on the menu after a chef transition). Score one for the mushroom challenge.
Though Hawk's Tavern closed in late 2012, chef Safir Rezzoug kindly sent over his recipe for this gorgeous salad. Consider this recipe as an excuse to buy some petite oven pans. Hunt for foraged mushrooms at the farmer's market. Perfect your poaching skills.
– Clean and cut the mushrooms any size you prefer but not too small, 1/2 ounces minimum.
*(DO NOT put the mushrooms in water because it will absorb it. Use a wet towel and gently clean the mushrooms).
– Separate the mushrooms by type in 3 different pans specific for oven.
– In each pan add 2 Tablespoons olive oil, 2 teaspoons raspberry vinegar and mix the mushrooms gently, add the 1 Tablespoon of salt in the end.
– Pre-heat the oven at 350°F. Roast the mushrooms between 10 to 15 minutes, depending on the thickness of mushrooms.
– Put water in the pan 1 ounce higher than the eggs, and bring to boil.
*(we want the eggs be warm not cold) and take out the shell gently.
– Slice the Yukon gold potato, in long and fine size, like strings.
– Pre-heat the fryer at 175°F with light colored canola oil.
– Make a little ball with the strings of potato and fry it.
*(The idea is to dry the potato with no coloration, for that we need to keep the temperature of the oil between 175°F and 185°F.
Use a spoon to keep the potatoes round like ball when fry it. The texture has to be very crispy.
– Mix all the ingredients together in a bowl (Italian parley, chive, tarragon, garlic, shallot, olive oil extra virgin and salt).
Make sure all the ingredients are cut to the same size for a good consistency and better taste.
– Make a hole in the middle of the mushrooms and place the poached eggs.
– Display the crispy potato on top of the egg with a pinch of salt.


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

	The mechanism sustaining the high-temperature corona \citep{Edlen43} and solar wind \citep{Parke58,Velli94} is still under investigation.
	Currently, it is widely accepted that the original energy source lies in the photpspheric convective motion and its interaction with magnetic fields \citep{Alfve47,Oster61,Stein98,Balle98,Fujim09,Kato011,Kato016}.
	Since the existence of Alfv\'en waves is indicated by in-situ observations \citep{Belch71a,Bale005} and remote sensing \citep{DePon07a,Tomcz07,Okamo11,McInt11,Thurg14},
	Alfv\'en-wave-driven models of the coronal heating \citep{Barne69,Cranm99} and solar wind acceleration \citep{Belch71b,Jacqu77} have been studied.
	Such models can explain the heating of both the coronal holes \citep{Hollw86,Suzuk05,Verdi10,Lione14,Matsu14,Balle16} and coronal loops \citep{Moriy04,Antol08,Balle11,Verdi12a}.
	Some models can explain the formation of both fast and slow solar winds \citep{Suzuk06a,Cranm07} by varying the expansion factor \citep{Wang090,Arge000}.

	To better model the corona and solar wind, the Alfv\'en wave propagation and dissipation needs to be solved precisely because the obtained structure is dependent on the heating distribution, that is, heating below and above the sonic point leads to slow and fast wind, respectively \citep{Hanst12}.
	To take into account heating mechanisms such as parametric decay \citep{DelZa01,DelZa15,Shi0017}, Alfv\'en wave turbulence \citep{Irosh64,Kraic65,Velli89,Goldr95,Matth99} and phase mixing \citep{Heyva83},
	we need to solve the three-dimensional compressible MHD equations with a sufficiently high resolution.
	However, due to its numerical difficulty and physical complexity, no models have ever included all the heating processes.
	To simplify the physics and reduce the computational cost, reduced MHD models have frequently been used \citep{Matth99,Dmitr02,Ought06,Cranm07,Verdi09,Chand09a,Verdi10,Perez13,Lione14,Balle16}.
	In such models, Alfv\'en wave turbulence driven by partial wave reflection \citep{Ferra58,Heine80,An00090,Velli93,Hollw07} is the only heating process.
	Some reflection-driven Alfv\'en wave turbulence models self-consistently succeed in explaining the coronal heating and solar wind accelerations \citep{Cranm07,Verdi10}.
	Recent 3D models, however, indicate that, under a smooth background field, turbulence cannot supply enough energy to sustain the corona \citep{Perez13,Balle17}.
	This indicates that we need to take into account the compressibility of plasma.
	In fact, compressible MHD models excluding Alfv\'en wave turbulence also succeed in generating the corona and solar wind \citep{Suzuk04,Suzuk05} based on shock heating.
	To summarize these recent studies, we need to solve for both shock (compressibility) and turbulence to achieve realisitc models.
	In this study, to solve both shock and turbulence heating without expensive numerical cost, we constructed a new 1D model of the coronal heating and solar wind acceleration.
	We solve the 1D compressible MHD equations to include shock formation and dissipation, and a one-point closure model is incorporated to include turbulence heating.
	The one-dimensionality and the resulting low numerical cost enable us to conduct a parameter survey to achieve a better understanding of the relevant physics.
	In this study, we investigate which type of heating is dominant in the corona and solar wind.

	The remainder of this paper is organized as follows.
	In Section \ref{sec:method}, we discuss how to incorporate turbulent dissipation into one-dimensional MHD equations.
	The basic equations and numerical solver are also described in this section.
	The results are shown in Section \ref{sec:result}, and we summarize the paper with a discussion in Section \ref{sec:summary_discussion}.

\section{Method} \label{sec:method}

\subsection{Phenomenological terms of Alfv\'en wave turbulence}\label{sec:method:dissipation}

        We consider a one-dimensional system with its coordinate curved along the background flux tube.
        We denote the coordinate along the tube by $r$; therefore, $\partial/\partial r \ne 0$.
        In this case, following \citet{Suzuk05,Suzuk06a}, the basic equations for the transverse velocity $\vec{v}_\perp$ and magnetic field $\vec{B}_\perp$ are given as
        \begin{align}
          &\rho \frac{d}{dt} \left( \sqrt{A} \vec{v}_\perp \right) = \frac{B_r}{4 \pi} \frac{\partial}{\partial r} \left( \sqrt{A} \vec{B}_\perp \right), \\
          &\frac{\partial}{\partial t} \vec{B}_\perp = \frac{1}{\sqrt{A}} \frac{\partial}{\partial r} \left[ \sqrt{A} \left( \vec{v}_\perp B_r - v_r \vec{B}_\perp \right) \right],
        \end{align}
        where, in this subsection, we use $A$ instead of $r^2 f$ to denote the cross section of the tube.
        $d/dt$ represents the Lagrangian derivative: $d/dt = \partial/\partial t + v_r \partial/\partial r$.
        Using the mass conservation and solenoidal condition,
        \begin{align}
          \frac{d}{dt} \rho + \frac{\rho}{A} \frac{\partial}{\partial r} \left( A v_r \right) = 0, \ \ \ \ \frac{\partial}{\partial r} \left( A B_r \right) = 0,
        \end{align}
        and taking into account the turbulent diffusivity, the equations for $\vec{v}_\perp$ and $\vec{B}_\perp$ are written as
        \begin{align}
          &\frac{\partial}{\partial t} \left( \rho \vec{v}_\perp A^{3/2} \right)
          + \left[ \left( \rho v_r \vec{v}_\perp - \frac{1}{4 \pi} B_r \vec{B}_\perp \right) A^{3/2} \right] \nonumber \\
          & = - \hat{\vec{\eta}}_1 \cdot \rho \vec{v}_\perp A^{3/2} - \hat{\vec{\eta}}_2 \cdot \sqrt{\frac{\rho}{4 \pi}} \vec{B}_\perp A^{3/2} , \label{eq:vperp_mod} \\
          &\frac{\partial}{\partial t} \left( \vec{B}_\perp A^{1/2} \right)
          + \frac{\partial}{\partial r} \left[ \left( v_r \vec{B}_\perp - \vec{v}_\perp B_r \right) A^{1/2} \right] \nonumber \\
          & = -  \hat{\vec{\eta}}_1 \cdot \vec{B}_\perp A^{1/2} - \hat{\vec{\eta}}_2 \cdot \sqrt{4 \pi \rho} \vec{v}_\perp A^{1/2}, \label{eq:bperp_mod}
        \end{align}
        where $\hat{\vec{\eta}}_1$ and $\hat{\vec{\eta}}_2$ are diagonal matrices whose components are given as
        \begin{align}
          &\hat{\vec{\eta}}_1=
          \left(
          \begin{array}{cc}
            \dfrac{c_d}{4 \lambda} \left( |\zeta^+_x| + |\zeta^-_x| \right) & 0 \\
            0 & \dfrac{c_d}{4 \lambda} \left( |\zeta^+_y| + |\zeta^-_y| \right) \\
          \end{array}
          \right), \\
          &\hat{\vec{\eta}}_2=
          \left(
          \begin{array}{cc}
            \dfrac{c_d}{4 \lambda} \left( |\zeta^+_x| - |\zeta^-_x| \right) & 0 \\
            0 & \dfrac{c_d}{4 \lambda} \left( |\zeta^+_y| - |\zeta^-_y| \right) \\
          \end{array}
          \right),
        \end{align}
        where $\lambda$ is the correlation length perpendicular to the mean field, $x$ and $y$ denote the two transverse components, and $\zeta$ represents the Els\"asser variables \citep{Elsas50} given by
        \begin{align}
          \vec{\zeta^{\pm}} = \vec{v}_\perp \mp \frac{\vec{B}_\perp}{\sqrt{4 \pi \rho}}.
        \end{align}
        Physically, $\hat{\vec{\eta}}_1$ represents a simple dissipation by turbulence, while $\hat{\vec{\eta}}_2$ comes from a relaxation process called dynamic alignment \citep{Dobro80,Strib91}.
	In fact, $\hat{\vec{\eta}}_2$ arises only for imbalanced turbulence \citep{Berez08,Chand08}.

        Here, we show that, as long as the density and radial velocity are time-independent as is often assumed,
        Eqs. (\ref{eq:vperp_mod}) and (\ref{eq:bperp_mod}) are consistent with the common Alfv\'en wave turbulence term.
        Introducing $\vec{b} = \vec{B}/\sqrt{4 \pi \rho}$, we can rewrite eq.s (\ref{eq:vperp_mod}) and (\ref{eq:bperp_mod}) as
        \begin{align}
          &\frac{\partial}{\partial t} \vec{v}_\perp + v_r \frac{\partial}{\partial r} \vec{v}_\perp - b_r \frac{\partial}{\partial r} \vec{b}_\perp \nonumber \\
          + &v_r \vec{v}_\perp \frac{\partial}{\partial r} \ln \left(  A^{1/2} \right) - b_r \vec{b}_\perp \frac{\partial}{\partial r} \ln \left( \rho^{1/2} A^{1/2} \right) \nonumber \\
          =& -\hat{\vec{\eta}}_1 \cdot \vec{v}_\perp - \hat{\vec{\eta}}_2 \cdot \vec{b}_\perp, \\
          &\frac{\partial}{\partial t} \vec{b}_\perp + v_r \frac{\partial}{\partial r} \vec{b}_\perp - b_r \frac{\partial}{\partial r} \vec{v}_\perp \nonumber \\
          + &b_r \vec{v}_\perp \frac{\partial}{\partial r} \ln \left(  A^{1/2} \right) - v_r \vec{b}_\perp \frac{\partial}{\partial r} \ln \left( \rho^{1/2} A^{1/2} \right) \nonumber \\
          =& -\hat{\vec{\eta}}_1 \cdot \vec{b}_\perp - \hat{\vec{\eta}}_2 \cdot \vec{v}_\perp.
        \end{align}
        These equations are written in Els\"asser variables as
        \begin{align}
          &\frac{\partial}{\partial t} \vec{\zeta}^{\pm} + \left( v_r \pm b_r \right) \frac{\partial}{\partial r} \vec{\zeta}^{\pm}, \nonumber \\
          - & \vec{\zeta}^{\pm} \left(v_r \mp b_r \right) \frac{\partial}{\partial r} \ln \left( \rho^{1/4} \right)
          + \vec{\zeta}^{\mp} \left( v_r \mp b_r \right) \frac{\partial}{\partial r} \ln \left( \rho^{1/4} A^{1/2} \right) \nonumber \\
          &= - \hat{\vec{\eta}}^{\mp} \cdot \vec{\zeta}^{\pm}, \label{eq:ho80_mod}
        \end{align}
        where
        \begin{align}
          \hat{\vec{\eta}}^{\mp} = \hat{\vec{\eta}}_1 \mp \hat{\vec{\eta}}_2 =
          \left(
          \begin{array}{cc}
            \dfrac{c_d}{2 \lambda} |\zeta^\mp_x| & 0 \\
            0 & \dfrac{c_d}{2 \lambda}  |\zeta^\mp_y| \\
          \end{array}
          \right).
        \end{align}
        Note that $v_r$ and $b_r$ represent the background flow speed and the Alfv\'en velocity, respectively.
        The left hand side of Eq. (\ref{eq:ho80_mod}) is identical to Eqs. (4a) and (4b) in \citet{Heine80}.
        The right hand side is equivalent to the Alfv\'en wave turbulence term approximated as \citep{Dobro80,Hossa95,Matth99}
        \begin{align}
		- \left( \vec{\zeta}^{\mp} \cdot \vec{\nabla} \right) \vec{\zeta}^{\pm} \sim - c_d \frac{Z^{\mp}}{2\lambda} \vec{\zeta}^{\pm},
		\label{eq:dissipation}
	\end{align}
        where $Z^{\mp}$ is the rms amplitude of $\zeta^{\mp}$, which is, following \citet{Chand09a} and \citet{Lione14}, approximated by $|\zeta^{\mp}|$ in this study.
        $\tau_{\rm turb}^{\pm} \sim \lambda/\zeta^{\mp}$ represents the timescale of the turbulence.
        The turbulence term $- \hat{\vec{\eta}}^{\mp} \cdot \vec{\zeta}^{\pm}$
        arises only when there exist counter-propagating Alfv\'en waves \citep{Irosh64,Kraic65}.
        The choice of $c_d$ is not trivial.
        Because the reflection timescale $\tau_{\rm ref}$ must be smaller than the nonlinear timescale $\tau_{\rm nl}$ to sustain the turbulence \citep{Dmitr03},
	\citet{Ought06} and \citet{Cranm07} evaluated $c_d$ as a function of the nonlinear timescale $\tau_{\rm nl}=\tau_{\rm turb}^{\pm}$ and the reflection timescale $\tau_{\rm ref}=\nabla \cdot \vec{V}_A$,
	which gives $c_d = 0$ for $\tau_{\rm nl} / \tau_{\rm ref} \to \infty$ and $c_d = 1$ for $\tau_{\rm nl} / \tau_{\rm ref} \to 0$.
	Meanwhile, \citet{Dmitr02}, \citet{Verdi07}, \citet{Chand09a}, \citet{Verdi10}, and \citet{Lione14} simply assume $c_d =1$.
 	Both models give similar results for the heating and acceleration, because $c_d$ is approximately unity for the main heating region in both cases.

        However, it has recently been pointed out by \citet{Balle11} and \citet{Balle16} that
        this formulation overestimates the turbulent dissipation than the value obtained from 3D calculations.
	\citet{Perez13} report that the heating rate calculated via 3D RMHD simulations is smaller compared to the required value.
	\citet{Balle17} conclude that $c_d=0.1$ gives a better approximation for the heating rate.
	Therefore, we use $c_d=0.1$ in this study.
	Note that the actual value or function of $c_d$ should have a complex form that depends on the structure of magnetic field and power spectrum, and thus $c_d$ is also a free parameter.
	However, because increasing $c_d$ is mathematically equivalent with decreasing $\lambda$, we fixed $c_d$ with a reasonable value by \citet{Balle17} and changed $\lambda$ in this study.

\subsection{Basic equations}

        In addition to Eqs. (\ref{eq:vperp_mod}) and (\ref{eq:bperp_mod}), we solve the mass conservation equation, the equation of radial motion, and the energy equation.
        The basic equations in conservation form are

	\begin{align}
		&\frac{\partial}{\partial t} \left( \rho r^2 f \right) + \frac{\partial }{\partial r} \left( \rho v_r r^2 f \right) =0,  \label{eq:mass} \\
    		&\frac{\partial}{\partial t} \left( \rho v_r r^2 f \right) + \frac{\partial }{\partial r} \left[ \left( \rho {v_r}^2 + p + \frac{{\vec{B}_{\perp}}^2}{8\pi} \right) r^2 f \right] \nonumber \\
    		&= \left( p + \frac{\rho {\vec{v}_{\perp}}^2}{2} \right) \frac{d}{dr} \left( r^2 f \right) - \rho g r^2 f, \label{eq:eomradial} \\
    		&\frac{\partial}{\partial t} \left( \rho \vec{v}_{\perp} r^3 f^{3/2} \right) + \frac{\partial }{\partial r} \left[ \left( \rho v_r \vec{v}_{\perp} - \frac{B_r \vec{B}_{\perp}}{4 \pi} \right) r^3 f^{3/2} \right] \nonumber \\
   		&= -\hat{\vec{\eta}}_1 \cdot \rho \vec{v}_{\perp} r^3 f^{3/2} - \hat{\vec{\eta}}_2 \cdot \sqrt{\frac{\rho}{4 \pi}} \vec{B}_{\perp} r^3 f^{3/2}, \label{eq:vt} \\
    		&\frac{\partial}{\partial t} \left(\vec{B}_{\perp}  r \sqrt{f}  \right) + \frac{\partial }{\partial r} \left[ \left( \vec{B}_{\perp} v_r - B_r \vec{v}_{\perp} \right) r \sqrt{f} \right] \nonumber \\
		&= -\hat{\vec{\eta}}_1 \cdot \vec{B}_{\perp} r \sqrt{f} - \hat{\vec{\eta}}_2 \cdot \sqrt{4 \pi \rho} \vec{v}_{\perp} r \sqrt{f}, \label{eq:bt} \\
   	 	&\frac{d}{dr} \left(B_r  r^2 f  \right) = 0, \label{eq:divb} \\
  		&\frac{\partial}{\partial t} \left[ \left( e + \frac{1}{2} \rho \vec{v}^2 + \frac{\vec{B}^2}{8 \pi} \right) r^2 f \right] \nonumber \\
  		&+ \frac{\partial }{\partial r} \left[\left( e + p + \frac{1}{2} \rho \vec{v}^2  + \frac{{\vec{B}_{\perp}}^2}{4 \pi} \right ) v_r r^2 f - B_r \frac{\vec{B}_{\perp} \cdot \vec{v}_{\perp}}{4 \pi} r^2 f \right] \nonumber \\
    		&= r^2 f \left( - \rho g v_r + Q_{\rm rad} + Q_{\rm cond}  \right), \label{eq:energy} \\
		& e = \frac{p}{\gamma-1}, \ \ \ \ p = \frac{\rho k_B T}{\mu m_H}, \label{eq:eos}
	\end{align}
	where $r$ is the heliocentric distance and $f$ is the expansion factor of the flux tube \citep{Kopp076,Wang090}.
	See \citet{Shoda18} for derivation.
        Note that Eqs. (\ref{eq:vt}) and (\ref{eq:bt}) are equivalent to Eqs. (\ref{eq:vperp_mod}) and (\ref{eq:bperp_mod}).
	$Q_{\rm rad}$ and $Q_{\rm cond}$ denote the radiative cooling and thermal conduction, respectively.
	The gravitational acceleration is $g = 2.74 \times 10^4 \left( r/R_{\rm Sun} \right)^{-2} {\rm \ cm \ s^{-2}} $.
	We assume that the solar atmosphere is composed of only hydrogen.
	$\mu$ is given as a function of density so that $\mu=1$ in the photosphere and low chromosphere and $\mu=0.5$ in the high chromosphere and corona.
	We ignored the dependence of $\mu$ on temperature for simplicity.
	Because we are interested in the coronal physics, and $\mu = 0.5$ (fully ionized) for coronal mass density, our assumption should not affect the numerical results.

	Following \citet{Suzuk05}, we assume a two-step super-radial expansion of the flux tube such that
	\begin{align}
		f = \frac{f_{\rm max,1} \exp \left( \frac{r - R_1}{\sigma_1} \right) + f_1}{\exp \left( \frac{r - R_1}{\sigma_1} \right)+1}
		\cdot \frac{f_{\rm max,2} \exp \left( \frac{r - R_2}{\sigma_2} \right) + f_2}{\exp \left( \frac{r - R_2}{\sigma_2} \right)+1},
	\end{align}
	where
	\begin{align}
		f_1 &= 1 - \left( f_{\rm max,1} -1 \right) \exp \left( \frac{R_{\rm Sun} - R_1}{\sigma_1} \right), \nonumber \\
		f_2 &= 1 - \left( f_{\rm max,2} -1 \right) \exp \left( \frac{R_{\rm Sun} - R_2}{\sigma_2} \right). \nonumber
	\end{align}
	The first and second terms represent the chromospheric and coronal expansions, respectively.
	We assume that the first expansion is near $r-R_{\rm Sun} = 1 {\rm \ Mm}$ with a length scale of $\sigma_1 = 0.25 {\rm \ Mm}$ while the second is near $r-R_{\rm Sun} = 200 {\rm \ Mm}$ with a length scale of $\sigma_2 = 350 {\rm \ Mm}$.
	The expansion factors  are $f_{\rm max,1}=120$ and $f_{\rm max,2} = 4$.
	The background magnetic field is calculated from $f$ as
	\begin{align}
		B_r = B_{r,0} \left( \frac{r}{R_{\rm Sun}} \right)^{-2} f^{-1}.
	\end{align}
	The correlation length is assumed to increase with the expansion of the flux tube \citep{Dmitr02}.
	In addition, to restrict the Alfv\'en wave turbulence to the corona \citep{Cranm07,Verdi10}, we formulate $\lambda$ such that
	\begin{align}
		\lambda  = \lambda_0 \sqrt{\frac{B_{r,0}}{B_r}} \max \left(1,\frac{\rho}{\rho_{\rm cor,1}} \right)  \label{eq:correlation},
	\end{align}
	where $\rho_{\rm cor,1} = 10^{-16} {\rm \ g \ cm^{-3}}$.
	This results in a turbulent dissipation slow enough to be negligible in the chromosphere.
	Note that some models indicate that the Alfv\'en wave turbulence is active also in the chromosphere \citep{Balle11,Verdi12a}.
	The purpose of this assumption is to compare our results to those of previous studies; there is no physical justification to exclude chromospheric Alfv\'en wave turbulence.

	Radiative cooling is a combination of optically thick $L_{\rm thick}$ and thin $L_{\rm thin}$ contributions and is given by
	\begin{align}
		Q_{\rm rad} = \xi L_{\rm thick} + (1-\xi) L_{\rm thin},
	\end{align}
	where
	\begin{align}
		\xi = \max \left[0,\left(1-\frac{\rho_{\rm cor,2}}{\rho} \right) \right].
	\end{align}
	Here, $\rho_{\rm cor,2} = 5 \times 10^{-17} {\rm \ g \ cm^{-3}}$.
	Following \citet{Gudik05}, instead of solving the radiative transfer, we approximate the optically thick cooling by Newtonian cooling as
	\begin{align}
		L_{\rm thick} = -\frac{1}{\tau_{\rm thick}} \left( e - e_0 \right),
	\end{align}
	where
	\begin{align}
		\tau_{\rm thick} = 1 \times \left( \frac{\rho}{\rho_0} \right)^{-1} {\rm \ s}, \ \ \ \ e_0 = \frac{1}{\gamma-1} \frac{\rho k_B T_{\rm ref}}{\mu m_H}.
	\end{align}
	Here, $\rho_0$ is the photospheric mass density and $\tau_{\rm thick}$ denotes the timescale of the cooling.
        $T_{\rm ref}$ represents a reference temperature that sets $T_{\rm ref}=6000 {\rm \ K}$ at $r = R_{\rm Sun}$ and monotonically decreases with $r$.
	As for $L_{\rm thin}$, we use the following formula:
	\begin{align}
  		L_{\rm thin} = - n_i n_e \Lambda(T), \ \ \ \ n_i = n_e = \frac{\rho}{m_H} \left(\frac{1}{\mu} -1 \right),
	\end{align}
	where we use an approximated loss function for $\Lambda(T)$ \citep{Suthe93,Matsu14}.

	In the chromosphere and low corona where the plasma is collisional, Spitzer-H\"arm conduction \citep{Spitz53} is applicable.
	However, in the solar wind, Spitzer-H\"arm conduction is inadequate due to the long mean free path, and thus free-streaming type conducton \citep{Hollw74,Hollw76} should be used instead.
	Because the free-streaming conductive flux is smaller than the Spitzer-H\"arm conductive flux, to mimic the transition to free-streaming conduction,
	we formulate the conductive heating $Q_{\rm cond}$ and conductive flux $q_{\rm cond}$ such that
	\begin{align}
		Q_{\rm cond} = - \frac{1}{r^2 f} \frac{\partial}{\partial r} \left( \alpha q_{\rm cond} r^2 f \right)
	\end{align}
	where
	\begin{align}
		q_{\rm cond} = - \kappa T^{5/2} \frac{\partial T}{\partial r}, \ \ \ \ \alpha = \max \left(1,\frac{\rho}{\rho_{\rm sw}} \right)
	\end{align}
	where $\rho_{\rm sw}=10^{-22} {\rm \ g \ cm^{-3}}$ and $\kappa=10^{-6}$ in CGS-Gaussian unit.
        $\alpha$ represents the flux quenching in the solar wind ($\rho < \rho_{\rm SW}$).

	\begin{figure}[!t]
	\vspace{3em}
	\begin{flushright}
	\includegraphics[width=80mm]{figure1.eps}
	\end{flushright}
	\vspace{-3em}
	\caption{
		Snapshots of altitudinal profiles for various $\lambda_0$.
		The mass density, temperature, radial velocity and transverse velocity are shown from the top to bottom,
		The red, orange, green and blue lines indicate
		$\lambda_0= 0.01 {\rm \ Mm}$, $\lambda_0= 0.1 {\rm \ Mm}$,
		$\lambda_0= 1 {\rm \ Mm}$, and $\lambda_0= 10 {\rm \ Mm}$, respectively.
										}
	\label{fig:result_compare}
	\end{figure}

\subsection{Boundary conditions and schemes}

        The basic equations are solved from the bottom (photosphere) up to $0.5 {\rm \ au}$ using 13000 non-uniform grid points.
        A static atmosphere with a temperature of $10000 {\rm \ K}$ is used as the initial condition \citep{Suzuk05}.
	The photospheric boundary conditions are as follows.
	The density, temperature, and radial magnetic field are fixed to $\rho_0 = 10^{-7} {\rm \ g \ cm^{-3}}$, $T_0 = 6000 {\rm \ K}$, and $B_{r,0} = 1000 {\rm \ G}$, respectively.
	The free boundary condition is applied to the radial velocity at the photosphere.
	The transverse velocity and magnetic field with pink-noise spectra are given at the photosphere so that upward waves are excited:
	\begin{align}
		\vec{v}_{\perp,0} &\propto \int_{2 \pi f_{\rm l}}^{2 \pi f_{\rm h}} d\omega \ \omega^{-1/2} \sin(\omega t + \phi(\omega) ), \\
		\vec{B}_{\perp,0}  &= - \sqrt{4 \pi \rho_0} \vec{v}_{\perp,0},
	\end{align}
	where $f_{\rm l}=10^{-3} {\rm \ Hz}$ and $f_{\rm h}=10^{-2} {\rm \ Hz}$.
        $\phi$ is a random function of $\omega$.
	The photospheric correlation length $\lambda_0$ and the root-mean-square value of $|\vec{v}_{\perp,0}|$ denoted by $\delta v_0$ are the free parameters in this study.
	As for the upper boundary condition, we apply the free boundary condition to every variable.
	Even though the transmitting boundary condition \citep{Thomp87,DelZa01,Suzuk06a} is likely better, we confirmed that the numerical result does not depend greatly on the boundary condition because a super-sonic and super-Alfv\'enic outflow is obtained as a final state.
	We solve the conservation law using an approximated Riemann solver \citep{Miyos05} with 2nd-order MUSCL reconstruction and 3rd-order TVD Runge-Kutta method \citep{Shu0088}.
	Super time stepping method \citep{Meyer12,Meyer14} is applied to solve the Spitzer-type thermal conduction in Eq. (\ref{eq:energy}), which drastically improves the calculation speed.

	\begin{figure}[!t]
	\vspace{3em}
	\begin{flushright}
	\includegraphics[width=80mm]{figure2.eps}
	\end{flushright}
	\vspace{-3em}
	\caption{
		Altitudinal profiles of the fractional density fluctuation $n$ and the normalized cross helicity $\sigma_c$.
		Shown by the four lines are cases with $\lambda_0=0.01{\rm \ Mm}$ (red),
		$\lambda_0=0.1{\rm \ Mm}$ (orange), $\lambda_0=1{\rm \ Mm}$ (green), and $\lambda_0=10{\rm \ Mm}$ (blue).
		Black circles indicate the radio-wave observations by \citet{Miyam14}.
				}
	\label{fig:ch_dro_compare}
	\end{figure}

\section{Result} \label{sec:result}

\subsection{Quasi-steady states for various $\lambda_0$ \label{subsec:qss}}

	Figure \ref{fig:result_compare} shows snapshots of the quasi-steady states for four cases with different $\lambda_0$ values.
	The photospheric transverse velocity is fixed to $\delta v_0 = 0.5 {\rm \ km \ s^{-1}}$.
	The panels show profiles of (a) the mass density, (b) temperature, (c) radial velocity, and (d) transverse velocity $v_t = |\vec{v}_\perp|$.
	The four lines indicate the results with $\lambda_0=0.01 {\rm \ Mm}$ (red),
	$\lambda_0=0.1 {\rm \ Mm}$ (orange), $\lambda_0=1 {\rm \ Mm}$ (green), and $\lambda_0=10 {\rm \ Mm}$ (blue).
	In each case, a chromosphere and corona are generated with a sharp transition region in-between them and a solar wind with velocity $\gtrsim 400 {\rm \ km\cdot sec^{-1}}$ is formed.

	Variations with respect to $\lambda_0$ will now be discussed.
	The solar wind has a different asymptotic velocity, which is larger for larger $\lambda_0$ (Figure \ref{fig:result_compare}c).
	The longer timescale of the turbulent dissipation makes waves propagate longer distances, giving rise to a faster solar wind because the heating in the supersonic region increases \citep{Lamer99,Hanst12}.
	The difference in the temperature profiles can also be interpreted via the location of the heating; the lower corona is hotter for smaller $\lambda_0$, while the wind is hotter for larger $\lambda_0$ (Figure \ref{fig:result_compare}b).
        As for the wave amplitudes (Figure \ref{fig:result_compare}d), the four cases show a similar trend.
	We see $v_t = 10-30 {\rm \ km \ s^{-1}}$ near the transition region and low corona, which is consistent with the observational values \citep{DePon07a,McInt11,Thurg14}.
	An increasing trend of $v_t$ up to $r/R_{\rm Sun}-1 \sim 3$ is seen in every case and is consistent with recent observation of non-thermal line broadening \citep{Baner09,Hahn013}.

	The density fluctuation and associated radial velocity fluctuation strongly depends on $\lambda_0$.
	The large density fluctuation, which was observed also in previous studies \citep{Suzuk05,Suzuk06a},
	comes from a large amplitude MHD slow (acoustic) waves generated via the parametric decay instability \citep{Sagde69,Golds78,DelZa01}.
	This is clear from the relationship between the time-averaged fractional density fluctuation $n$ and the normalized cross helicity $\sigma_c$ defined as
	\begin{align}
		n &= \frac{1}{\bar{\rho}}\sqrt{\overline{(\rho-\overline{\rho})^2}}, \\
		\sigma_c &= \frac{\overline{E^{+}}-\overline{E^{-}}}{\overline{E^{+}}+\overline{E^{-}}}, \ \ \ \ E^{\pm} = \frac{1}{4} \rho \vec{\zeta^{\pm}}^2,
	\end{align}
	where $\overline{X}$ denotes the time average: $\overline{X} = 1/\tau \int^\tau_0 dt X$, where $\tau=1000{\rm \ min.}$
	In Figure \ref{fig:ch_dro_compare} we show the altitudinal profiles of $n$(a) and $\sigma_c$(b).
        It is clear, especially for large $\lambda_0$, that the increasing $n$ is associated with decreasing $\sigma_c$, which is consistent with the parametric decay instability.

        \begin{figure*}[!t]
	\begin{flushright}
	\includegraphics[width=175mm]{figure3.eps}
	\end{flushright}
	\vspace{1em}
	\caption{
		Altitudinal profiles of the time-averaged total heating ($Q_{\rm heat}/\rho$: blue line) and turbulence heating ($Q_{\rm turb}/\rho$: red line) for various $\lambda_0$.
		The left, middle and right panels indicate $\lambda_0=0.1{\rm \ Mm}$, $\lambda_0=1{\rm \ Mm}$, and $\lambda_0=10{\rm \ Mm}$, respectively.
				}
	\vspace{1em}
	\label{fig:heating_pergram_compare}
	\end{figure*}

        According to Figure \ref{fig:ch_dro_compare}a, $n$ has maxima near $r/R_{\rm Sun}-1=10^{-2}$ (the chromosphere and transition region) and $r/R_{\rm Sun}=10$ (the solar wind).
	The first one results from sound waves nonlinearly generated from Alfv\'en waves via the wave pressure gradient \citep{Hollw71,Hollw82a,Kudoh99,Matsu10}.
	The sound waves are amplified due to the stratification and steepen to form shock waves \citep{Carls92,Tian014}, leading to large density fluctuations.
	After a shock wave collides with the transition region,
        its energy is redistributed to the coronal shock wave, the upward motion of the transition region, and the chromospheric rarefaction wave \citep{Hollw82b}.
	This is the cause of the rapid decrease in $n$ above the transition region.
	The second peak results from the decay instability, which enhances $n$ and reduces $\sigma_c$ due to backscattering \citep{Malar00,DelZa01,Shoda16}.

	The black circles in Figure \ref{fig:ch_dro_compare}a indicate radio-wave observations by \citet{Miyam14} using {\it Akatsuki} \citep{Nakam11}.
        All four cases show an increasing trend for $n$ with $r$ in $0.1<r/R_{\rm Sun} -1 \lesssim10$, which is consistent with the observation.
	These observational data could underestimate the actual values because positive and negative density fluctuations, which cause radio scintillation,
	are canceled out in the integration along the line of sight.
	Therefore, even though our theoretical results exceed most of the observational data, this discrepancy is not a contradiction.

	Even though the fluctuations in $\rho$ and $v_r$ has a large length scale typically of $0.1R_{\rm Sun}$,
	they are not observable by remote sensing because the intensity of that region is extremely low.
	In-situ observations would be the only way to detect the fluctuations, which is expected from {\it Parker Solar Probe} \citep{Fox0016}.

	$n$ and $\sigma_c$ show different behaviors with different $\lambda_0$.
	First, the magnitude of $n$ near $r/R_{\rm Sun}=10$ is smaller for smaller $\lambda_0$.
	This is likely because the growth rate and saturation level of the decay instability decrease due to smaller wave powers or because the decay instability itself is suppressed by the presence of turbulence.
	Second, the magnitude of $\sigma_c$ in the corona and solar wind becomes smaller as $\lambda_0$ increases.
	This is a natural result of dynamic alignment \citep{Dobro80,Strib91}.
	Large $\sigma_c$ observed in the fast solar wind near $1{\rm \ au}$ \citep{Belch71a,Bavas00} likely results from small $\lambda_0$ ($\lambda_0 \lesssim 0.1 {\rm \ Mm}$) and the subsequent alignment.
	However, recent observations by CoMP reveal that a significant amount of reflected Alfv\'en waves exist in the low corona \citep{Morto15}.
	According to \citet{Morto15}, the energy ratio $E^- / E^+$ is $0.5-1.0$, which is, in terms of $\sigma_c$, $0-0.3$.
	Thus, $\lambda_0\gtrsim 1 {\rm \ Mm}$ is preferable to explain their observation.
	Explaining the cross helicity profile from the low corona up to the distant heliosphere $r\gtrsim 1{\rm \ au}$ is beyond the scope of this study and remains for future work.

\subsection{Heating mechanism
	\label{sec:heating_mechanism}}

	To measure the heating, we use the energy equation written in the following manner \citep{Cranm07}.
	\begin{align}
		\frac{\partial e}{\partial t} + v_r \frac{\partial e}{\partial r} + \frac{e+p}{r^2 f} \frac{\partial}{\partial r} \left( v_r r^2 f \right) = Q_{\rm rad} + Q_{\rm cond} + Q_{\rm heat},
	\end{align}
	where $Q_{\rm heat}$ is the heating by waves.
	This equation is derived from the basic equations.
	After a quasi-steady state is achieved, using time averaging, we obtain
	\begin{align}
		\overline{Q_{\rm heat}} =
		\overline{v_r \frac{\partial e}{\partial r}  +\frac{e+p}{r^2 f} \frac{\partial}{\partial r} \left( v_r r^2 f \right) - Q_{\rm rad} - Q_{\rm cond}},
	\end{align}
        where we use $\overline{\partial e / \partial t}=0$.
	We can calculate the total wave heating in this manner.
	Meanwhile, the turbulent heating $Q_{\rm turb}$ is analytically derived as \citep{Verdi07,Cranm07}
	\begin{align}
		Q_{\rm turb} = \frac{1}{4} \rho \sum_{i=x,y} c_d \frac{|\zeta^{+}_i|{\zeta^{-}_i}^2+|\zeta^{-}_i|{\zeta^{+}_i}^2}{\lambda},
	\end{align}
	where $x$ and $y$ denote the components perpendicular to the background flux tube.
	In Figure \ref{fig:heating_pergram_compare}, we show the time-averaged heating per unit mass $\overline{Q_{\rm heat}}/\overline{\rho}$ (blue line)
	and $\overline{Q_{\rm turb}}/\overline{\rho}$ (red line) for cases with the same wave amplitude ($\delta v_0 = 0.5 {\rm \ km \ s^{-1}}$)
	and different correlation lengths ($\lambda_0=0.1 {\rm \ Mm}, 1{\rm \ Mm}, and 10{\rm \ Mm}$).
	In every case, the heating per unit mass reaches $\sim 10^{11} {\rm \ erg \ g^{-1} \ s^{-1}}$,
        showing that a sufficient amount of energy is supplied to sustain the coronal temperature.
	For $\lambda_0 \lesssim 0.1{\rm \ Mm}$, the turbulence heating is dominant everywhere; meanwhile for $\lambda_0 \gtrsim 1{\rm \ Mm}$, the shock heating is comparably or more important in the extended corona and solar wind.
	Thus our first conclusion is that the dominant heating process is turbulence when $\lambda_0 \lesssim 1{\rm \ Mm}$.
	In particular, when $\lambda_0 \lesssim 0.1 {\rm Mm}$, the shock heating is nearly negligible.
	What is interesting in this analysis is that, even though we apply small turbulence heating ($c_d = 0.1$),
        the sufficient amount of energy is supplied only by the turbulent heating when $\lambda_0= 1 {\rm \ Mm}$.
	In contrast, a reduced MHD calculation \citep{Perez13} gives a heating rate of at most $\sim 10^{10} {\rm \ erg \ g^{-1} \ s^{-1}}$ when $\lambda_0 \sim 1 {\rm \ Mm}$.
	The enhanced heating indicates that Alfv\'en wave reflection, which is the trigger of Alfv\'en wave turbulence, is activated due to the compressibility.
	This is possibly because of the presence of parametric decay or reflection driven by density fluctuations \citep{Suzuk06a,Balle16}.
	In this regard, the compressibility can never be ignorable not only due to shock heating but also due to reflection enhancement.

	\begin{figure*}[!t]
	\begin{flushright}
	\includegraphics[width=175mm]{figure4.eps}
	\end{flushright}
	\vspace{1em}
	\caption{
		Time-averaged wind velocity at $r=0.5 {\rm \ au}$ (left), maximum temperature (middle), and mass loss rate (right)
		for various $\lambda_0$ and $\delta v_0$.
		The units for the vertical axes are ${\rm km \ s^{-1}}$, ${\rm MK}$, and $M_{\rm Sun} \ \rm{ yr^{-1}}$, respectively, where $M_{\rm Sun}$ is the solar mass.
		The horizontal axis shows $\lambda_0$ in unit of ${\rm Mm}$.
		The red, green, and blue lines indicate $\delta v_0=0.4 {\rm \ km \ s^{-1}}$,
		$0.5 {\rm \ km \ s^{-1}}$, and $0.7 {\rm \ km \ s^{-1}}$, respectively.
		}
	\vspace{2em}
	\label{fig:corr_dependence}
	\end{figure*}

\subsection{Dependences on $\lambda_0$ and $\delta v_0$}

	Following \citet{Cranm07}, we discuss the dependences of the asymptotic solar wind velocity, maximum coronal temperature and mass loss rate
	on $\lambda_0$ and $\delta v_0$.
	We show in Figure \ref{fig:corr_dependence} the time-averaged (a) wind velocity at $r=0.5{\rm \ au}$, (b) maximum temperature and (c) mass loss rate.

	According to \citet{Cranm07} and \citet{Verdi10}, the solar wind velocity tends to increase when $\lambda_0$ increases.
	This is observed in our result regardless of $\delta v_0$.
	\citet{Cranm07} and \citet{Suzuk06a} also argue that the wind velocity decreases as $\delta v_0$ increases.
	This is evident for large $\lambda_0$.
	As for small $\lambda_0$, the wind velocity is nearly constant around $\sim 400 {\rm \ km\ s^{-1}}$,
	indicating that the solar wind is completely thermally driven \citep{Parke58,Hartl68}.
	The maximum temperature changes little with $\lambda_0$ and $\delta v_0$ as seen in \citet{Cranm07}.
	Especially, the maximum temperature is almost constant with respect to $\lambda_0$.
        This invariance is because the change in $\lambda_0$ is balanced by adjusting the fractional contributions from turbulence and shock heating.
        Indeed, the total heating rate per unit mass is nearly the same for different $\lambda_0$ values (Figure \ref{fig:heating_pergram_compare}).
        Suppose that $\lambda_0$ becomes smaller and turbulent heating is enhanced.
        Due to the increase in the coronal gas pressure, the plasma becomes more incompressible, leading to the reduction of compressible heating.
	The mass loss rate is also independent of $\lambda_0$, because it is almost independent of the heating location \citep{Hanst95}.
	Meanwhile, the mass loss rate sensitively depends on $\delta v_0$ \citep{Suzuk06b,Cranm07};
	the cases with $\delta v_0=0.7 {\rm \ km  \ s^{-1}}$ give approximately an order of magnitude larger mass loss rates than the cases with $\delta v_0=0.4 {\rm \ km  \ s^{-1}}$,
	even though the energy input $\propto \delta v_0^2$ is only three times larger.
	This is mainly because the reflection of the Alfv\'{e}n waves is suppressed for larger $\delta v_0$;
	a larger $\delta v_0$ gives higher coronal density and hotter corona because of the larger heating.
	The denser corona suppresses the wave reflection in the chromosphere because the density difference between the photosphere and the corona is smaller;
	the hotter corona suppresses the wave reflection in the corona because the scale height is larger there.
	These effects make a larger fraction of the input energy transmitted to the corona and the solar wind region to drive denser wind \citep{Suzuk13}.
	To summarize, our simulations obtain the same trends as those obtained by \citet{Cranm07}.
        This is not trivial because we include compressibile waves in the corona and solar wind and use different values for $c_d$.

\section{Summary \& Discussion} \label{sec:summary_discussion}

	In this paper, we proposed a new 1D model of the coronal heating and solar wind acceleration.
	Our model is a hybrid model of a time-dependent compressible heating model \citep{Suzuk05} and an incompressible heating model \citep{Lione14}.
	Because both the compressible heating and incompressible heating are important in the corona and solar wind \citep{Matsu14},
	our model likely gives a better result compared to previous studies.
	As shown in Figure \ref{fig:result_compare}, the corona and the solar wind are formed regardless of the photospheric correlation length $\lambda_0$.
	The main heating mechanism is the turbulence heating (Figure \ref{fig:heating_pergram_compare}), especially when $\lambda_0 \lesssim 1 {\rm \ Mm}$.
	This does not necessarily mean that the compressibility is negligible.
	The fact that we obtain sufficient amounts of turbulence heating even for $\lambda_0 = 1{\rm \ Mm}$ despite small $c_d$ ($c_d=0.1$) indicates that the compressibility plays a role in the enhancement of
	Alfv\'en wave reflection and, as a result, turbulence heating via the parametric decay instability.
	The density fluctuation, cross helicity, and solar wind velocity are strongly affected by $\lambda_0$ (Figure \ref{fig:result_compare}, \ref{fig:ch_dro_compare}),
	while the maximum coronal temperature and mass loss rate are almost independent of $\lambda_0$ (Figure \ref{fig:corr_dependence}).

	Our turbulence model is one of the simplest models currently in use, and there is much space for improvement.
	The turbulence term we used is derived from the reduced MHD equations \citep{Hossa95,Dmitr02}.
	However, this treatment may not be applicable to our compressible MHD system.
	For a better modeling, the direct treatment of the compressible MHD turbulence \citep{Grapp93,Chand05} may be a better approach.
	To discuss the spectral evolution in the wave-number space, a shell model \citep{Buchl07,Verdi12b} is a possible extension to solve a large range of spatial scales.

	The photospheric correlation length, $\lambda_0$, should in principle be determined from the physical properties of the magneto-convection below the photosphere.
	According to \citet{Rempe14}, the spatial power peak of the photospheric kinetic energy lies around $\lambda \sim 1{\rm \ Mm}$,
	while the magnetic energy is nearly flat for $0.1 {\rm \ Mm} \lesssim \lambda \lesssim 10 {\rm \ Mm}$.
	$\lambda \sim 1{\rm \ Mm}$ is on the scale of granulation while $\lambda \sim 0.1 {\rm \ Mm}$ corresponds to the scale of intergranular sub-arcsec magnetic patches \citep{Berge95,Berge01}.
	If we simply assume that $\lambda_0$ is comparable to the energetic scale of the photospheric motion, $\lambda_0=1{\rm \ Mm}$ is a reasonable choice.
	This assumption is equivalent to the idea that the swaying motion of the flux tube is the main driver of transverse waves \citep{Stein98}.
	However, if the vortex flow inside the magnetic patches is the most energetic driver of transverse waves \citep{Balle11},  $\lambda_0=0.1{\rm \ Mm}$ is preferable.
	Radiation MHD simulations indicate that the vortex size in the chromosphere is around $\lambda \sim 1{\rm \ Mm}$ \citep{Moll012,Iijim17}.
	Therefore, the most preferable value of $\lambda_0$ lies between $0.1 {\rm \ Mm}$  and $1 {\rm \ Mm}$, depending on the generation mechanism of waves.
	As discussed in Section \ref{subsec:qss}, the coronal observation is consistent with $\lambda_0 \gtrsim 1 {\rm \ Mm}$.
	Thus, $\lambda_0 \sim 1 {\rm \ Mm}$ is consistent with the photospheric wave driving and coronal wave observation,
	although the best choice for $\lambda_0$ should be investigated in detail from both aspects in future works.

	M.S. is supported by Leading Graduate Course for Frontiers of Mathematical Sciences and Physics (FMSP) and  Grant-in-Aid for JSPS Fellows.
	T.Y. is supported by JSPS KAKENHI Grant Number 15H03640.
	T.K.S. is supported in part by Grants-in-Aid for Scientific Research from the MEXT of Japan, 17H01105.
	Numerical calculations were in part carried out on PC cluster at Center for Computational Astrophysics, National Astronomical Observatory of Japan.

redpajama_set_name: RedPajamaArXiv


We'd sat next to each other in the same row of cubicles for a year. We regularly talked about our weekend plans, helped each other out with tough assignments, and vented to each other about office drama. She was a great co-worker, and we worked together flawlessly.
Then, one day, everything changed—she become my manager.
In a swift department shift, she was promoted, and I become one of her direct reports.
If you're ever in the same situation, it can be hard to fight through the range of emotions you're feeling—everything from being proud of your co-worker to wanting to rip that lofty title right out of her hands. But to make the move successful for everyone involved, you need to do these key things.
I know what you're thinking: It's not fair that your co-worker got the promotion, you deserve to be the manager, he or she gets an office while you're stuck in a tiny cube, and he or she probably got a giant raise.
I know, because I thought those things, too.
It's going to be hard to face your co-worker's new managerial position without at least a twinge of jealousy. No matter how happy you are for him or her or how great the two of you get along, a little envy is inescapable.
But get those thoughts out of the way now, because at the end of the day, this is the situation you're in, and jealousy won't change it. With the right attitude, you can use that jealousy in a healthy way to benefit your career—but don't let it get in the way of your success in your company and under your new manager.
As I've mentioned, in this new situation, your thinking is probably already on the selfish side. Rather than thinking about how wonderful it is that your friend got a promotion, for example, you're probably feeling sorry for yourself and your inhibited work friendship.
Well, good news: I'm here to tell you to continue on that self-centered road and start to consider how your co-worker's promotion can benefit you.
Remember all those things you and your co-worker vented to each other about when you were cubemates? Maybe you thought a department policy was inefficient or that employees should have more flexibility to work from home. Guess what? Now that your co-worker is in a position of power, he or she may actually be able to make those changes happen.
I remember complaining to my co-worker that I'd had almost no communication with Rebecca, our chief marketing officer. When that co-worker became my manager, the first thing she said was, "I have a one-on-one meeting with Rebecca today; do you want me to get you some time on her calendar?" And voilà—I finally had a direct line of communication to the CMO.
Remember: Your co-worker has literally been in your position before—she understands what you want and is now in a position to make that happen. Take advantage of it!
When my co-worker became my boss, I immediately started looking at everything she did through a tainted lens. She wanted to review my draft before I continued with a project? Obviously, she was a micromanager. She started assigning me projects and reminding me of deadlines? Clearly, she was on an out-of-control power trip.
In the heat of the moment, it can be easy to perceive certain events or behaviors in a skewed way. But let's be realistic: As a manager, doling out assignments and reviewing her employees' work is part of her job. All she's doing is stepping up to her role and doing what's expected of her—and you can't blame her for that.
Instead of intentionally looking for things to blame her for, give her the benefit of the doubt. Wait to see how things play out.
Right off the bat, some things may be different about your day-to-day relationship.
For example, my co-worker and I used to vent to each other about Matt, the manager of a department we worked closely with. Whenever one of us had to interact with him, we'd share all the gory details with the other.
But once she become my manager—and a peer of Matt's—she wasn't quite as open. Now that she was working with him on a daily basis, she had to maintain a good relationship with him, and she realized she couldn't be speaking down about him to her team. All of a sudden, our venting sessions changed. I sensed that she took her managerial role very seriously, and didn't want to risk her professionalism by gossiping.
That particular element of our relationship simply had to change—but for the sake of my co-worker's career (and mine), it was probably for the best.
On the other hand, it's important to realize that not everything about your relationship has to change.
Maybe, as co-workers, you used to go to lunch once a month. That's something that doesn't necessarily have to stop, as long as your co-worker-turned-manager knows how to navigate the sometimes-tricky waters of being friends with employees without playing favorites (and if he or she doesn't, here are some tips).
Yes, you need to be respectful of your co-worker's new role—but as long as you tread carefully, you don't have to start your professional relationship from scratch.
It's understandably tough to see the working relationship between you and your co-worker change.
But as career coach Lea McLeod often says, it's your job to make your manager more successful. And that doesn't change just because your boss is your former co-worker.
It does, however, make that goal a little easier. So often, employees struggle with figuring out how to work effectively with their managers—how to communicate successfully, disagree respectfully, and ask for help when they're confused. Well, after working with this person for so long, you should have those things down to a science. And that will make your job much easier.
Yes, reporting to a co-worker may feel awkward at first, but when you handle it in a professional, respectful manner, everyone will win.
Photo of goldfish jumping courtesy of Shutterstock.


Julie Hendicott, Lois Birk, Caroline Glass-Pattison and Bruce Lowrie are members of the Guringai Aboriginal Educational Consultative Group. They describe their different links to this place and how they are working to bring awareness of Aboriginal culture, values and perspectives into the school system. These are tasks of education, validation and community building.


Liberty's Lauren Hofer (32) puts up a shot over the outstretched arm of Orange's Hannah Sargent (12) during the first half of Friday's Division I sectional final in Powell.
Breanna Yashko jump-started a 12-2 run to open the second half to help Olentangy Liberty defeat rival Olentangy Orange 48-32 in the second round of the Division I girls basketball district tournament Friday night in Powell.
Yashko, who led the way with 14 points, assisted Savitha Jayaraman for three to open the third-period scoring before she hit one of her own — three of seven consecutive points she scored for the Patriots.
"I think when Yashko is right, our team is right," Jayaraman said.
Yashko was held to two points in the first half.
Gracie Foth capped the run with a steal and a layup to give Liberty (21-3) a 31-16 lead with about three and a half minutes left in the third. The Patriots led 38-22 through three.
Liberty was held scoreless from the field in the fourth quarter, but proved why free throw shooting is important. The Patriots went a perfect 10-for-10 from the line, including an 8-for-8 performance by senior post Lauren Hofer.
"We didn't really need to hit a shot from the field in the fourth quarter," Krafty said.
The Patriots also started strong from the line, going 5-for-6 in the first period to spark a 9-2 lead through one. They finished 20-of-23 while Hofer scored 11 of her 13 points at the line with just one miss. Hofer had a team-high four steals.
Free throw shooting may have been the key to the Patriots scoring, but defensively Jayaraman blocked three shots on one possession. She finished with seven blocks to go with 10 points.
Orange (10-13) came storming back with seven straight points to open the second. McKenna Ford hit a three-pointer to start the rally and freshman Courtney Scott capped the run with a steal and a score to tie it 9-9 with 4:46 left in the half.
Courtney Scott drove the lane and scored to make it a two point deficit at 16-14, but Gracie Foth banked in a three-pointer to give Liberty its 19-14 lead at the break.
Hannah Sargent had 10 points and four rebounds, Ford finished with eight points and seven rebounds and Scott added seven points and four steals for the Pioneers.
"You gotta expect that everybody is going to give (Liberty) their best shot, and we were going to give them a better shot than we did the last time," Bob Scott said.
Liberty defeated Orange 84-46 at home Dec. 16.
Next up, Liberty plays 11th-seeded and OCC-Central rival Upper Arlington in the district semifinal Wednesday night at 7 p.m. at a site to be determined.
http://aimmedianetwork.com/wp-content/uploads/sites/40/2016/02/web1_patriots00-1.jpgLiberty's Lauren Hofer (32) puts up a shot over the outstretched arm of Orange's Hannah Sargent (12) during the first half of Friday's Division I sectional final in Powell.


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A woman says she was terrified when a stranger stopped her car and tried to get into her passenger seat in Littleover.
The woman, who does not wish to be identified, claims she was travelling down Pastures Hill when the vehicle in front of her stopped suddenly as though to avoid something or someone.
She then says a man ran towards her car and put his hands on her bonnet, gesturing at her to stop.
The woman says she panicked and attempted to put her car into reverse while the stranger ran towards the passenger side and pulled the door handle.
Fortunately, she says the man failed to open the door as her car locks automatically from the inside when driving.
She said: "He was pulling at the door handle and I think he was just saying 'please' over and over again so I just shook my head and drove off.
"I had to drive on the opposite side of the road because he was still in the road and there was bollards and lights and then traffic lights so I couldn't stay on my side of the road."
Panicked, the woman said she even drove the wrong way around a roundabout to get away from the man when she came across another car with its windows down.
She then says she asked the driver if she knew the man and claims he replied 'yes' before speeding away.
She continued: "My first thought is that I should help him but then I thought no, I've got to think about myself.
"Since then I've thought he might have been trying to steal my car, that's what a lot of other people have said too."
The pedestrian and the man in the car are being described as white, in their 30s and both having dark hair and stubble.
The pedestrian was wearing jeans and a dark jacket.
The woman said she had reported the incident to police.


text:
The Meaning of Love in Other Cultures
mallie Aprile 9, 2022 Uncategorized
Do you know the which means of love in other cultures? Various people have problems interpreting feelings that they encounter as appreciate. In fact , research has shown that love is actually a universal emotion, but it is usually expressed differently in different cultures. The basic thoughts theory of emotion, known as the Basic Emotions, argues which we recognize every single basic feelings by it is invariable facial expression. However , absolutely adore in other cultures has some unusual associations. Listed below are some of the dissimilarities between absolutely adore in Uk and love in other cultures.
The Urhobo people of Nigeria possess unique cultural practices that reflect that they view take pleasure in. One of these traditions involves the bride price, also called a dowry, which is paid out to the category of the intended husband by the son. In return, the son's family will offer the group of the potential bride products and libations for the parents of the near future wife. The son need to then get hold of his young one's consent to marry her before the method can carry on.
A report conducted simply by Robin Goodwin and Charlotte now Findlay more than a decade ago found that Chinese individuals were very likely to express their feelings of affection for their partners than have American participants. This might have got something to do with the actual fact that the cultures have a circular look at of time. As opposed, the Japanese traditions requires the perfect time to fall in love and openly ask for someone. In Photography equipment cultures, like is often expressed through a ritual that involves time spent between in-laws.
If you're an intimate or a creature lover, the nature of love is carefully linked with natural splendor. Ancient philosophers closely linked beauty and love. 1 Greek fable explains that the rose made an appearance at the moment Morgenstern was born. One other painting by simply Botticelli describes the goddess of springtime preparing Venus in plants. As a result, blossoms are associated with love and beauty. You will be surprised to find out that the Greeks were not the first people to associate magnificence with love.
Esther's dad is polygamous, with three wives and 21 children. The Maasai practice polygyny, which is prevalent among pastoralists, seems a paradox just for Westerners so, who believe in real love. A BASSE CONSOMMATION reporter once asked Maasai teenage males to determine love. That they replied with a shy guffaw and shrugged their brain. They rarely seem to figure out our notion of love.
Love consist of cultures has evolved as a general emotion. In ancient Portugal and The italian capital, girls were elevated into a more dignified status than boys. The ancient Greeks and Romans considered love to be a way to discover yourself. The Ancient greek language philosopher Aristophanes argued that https://yourbrideglobal.com/ukrainian-brides-sites/ absolutely adore is an unrequited hunt for the home. Moreover, the reunion of Odysseus and Penelope in the Odyssey may be a miniature enchantment novel with all its qualities of camaraderie, courtship, and sex mutuality.
In Latina America, like is characterized by language. In Spanish, you will find two ways they are required "I absolutely adore you. " While "te quiero" is used pertaining to friends and family, "te amo" is certainly reserved for specialized people. If you would like to tell somebody in The spanish language that you just love them, you employ the phrase "te amo, " which is even more romantic and reserved for an associate. Then you can just say "I love you" in another dialect.
Love stories in other cultures can be amazing. Sometimes scientists find stories about absolutely adore in other nationalities, but the stories are very totally different from what we typically see in the West. While the effect of the European culture is largely due to its economical, navy, and politics hegemony, it is also a ethnical feature that is wide-spread. We share our emotions by using heart and soul symbols, emoting with "I love you" and partying Valentine's Day.
Valentine's Day would not exist in Romania. The holiday is commemorated in March one particular instead. It really is similar to Valentine's in that men often provide their smash a porcelain figurine, although it has become incredible into a more generic treat of a ribbon and bow. Romanian life is remarkably patriarchal, with males approaching girls almost solely. Moreover, what "I like you" are much more reserved in other cultures, and are available to family members and friends.
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For most people a car is the second most significant purchase they will ever make after their home. Buyers often spend weeks and months hunting out their perfect car – but oddly, most don't put a similar effort into sourcing the right car finance deal.
Research shows that buyers often spend huge amounts of time shopping around several dealerships for the best bargains and will then haggle over relatively small issues such as a tank of petrol or a spare tyre. However many then simply agree to the first finance agreement that is offered to them.
Choosing the wrong finance deal for your vehicle can be costly. Research undertaken by a senior financial watchdog found that more than 80% of used vehicles are bought using finance deals offered by the seller. This results in many buyers paying around £1,000 extra over the loan term than they would have had done if they had shopped around.
Car dealers will sometimes offer to reduce the price of the car if the buyer takes out finance through them. This is often a false economy but seems like a good deal at the time. Without all of the figures in front of you, it is very hard to work out what the best deal is so don't sign without considering other options.
How do Savvy Buyers find the Best Finance Deals?
Firstly – and most importantly – they shop around. There are now lots of independent car finance providers, such as justcarfinance and it is worth contacting a number of potential lenders to ask for a quote. The deregulation of the finance industry had led to more competition and this has helped with the cost of finance coming right down. This is obviously good news for buyers – but only if you are prepared to hunt out the best deals.
Buyers need to consider the amount they can afford to spend on their car every month. Of course there is always a pay-off between reducing the amount of the monthly repayments and increasing the repayment period. If you take a loan over a longer period, it obviously increases the overall amount of interest to be paid back. It is best to pay as much back every month as you can afford but this needs to be calculated using an honest and reliable budget. Budgets prepared by most buyers tend to be very optimistic.
Even if a dealer offers an upgrade or discount for taking their in-house finance, you must do your sums to make sure that it offers the cheaper option overall.
If you receive a windfall, it is usually possible to pay off a chunk of any remaining debt. Often there is a charge for this, but it may still be worth it if it reduces the overall interest.
Those with a low credit rating may find it more difficult to secure a finance package and if they are accepted by a lender, they may be charged a higher rate of interest. In this case it is even more important to shop around as there are now many of companies catering for those with poor credit ratings.


potency of the poison varied by location: most potent in the Willamette Valley of Oregon and decreasing in potency as one goes north.
These photos were taken at Ridgefield, a wildlife reserve in Southern Washington, so it is unclear how poisonous the newt would be, but there is a good chance that was the duck's last meal.
When most people see one of these ducks they think it should be called a Ring-billed Duck. The first photo is of a Drake and shows that, in fact, there really is a ring around the neck.
The other photos show the hen eating the newt.
This entry was written by whyevolutionistrue and posted on March 23, 2018 at 8:00 am and filed under birds, herps and amphibians, photography. Bookmark the permalink. Follow any comments here with the RSS feed for this post.	Both comments and trackbacks are currently closed.
I bet the dinosaur ducks have some ability to deal with the newt poison so they do not succumb. Would a heron die?
Ah – I see from the link it would!Poor duck!
The old conundrum – if fatal, the ducks may never learn that the newt is bad, & so will continue to scoff them when they see them. Surely it is more advantageous to just taste disgusting?
But…each duck that eats rough-skinned newts never eats another one (unless they have an immunity). So only the ducks that do not eat these newts survive to reproduce.
Amazingly John's pics above were scraped by Googlebot & put up in image search at 13:09 GMT – not far behind the post going up. WEIT must have high 'crawlability' or just happened to coincide with a bot visit.
I'm having trouble with the duck being a dead duck! I read of a similar incident with a mallard duck on Bee's, Birds & Butterflies & the naturalist reported the duck continued going about its business for some time after – no time given. This was in the Greater Olympia area, WA. Why didn't the duck refuse the prey given the 'orrible taste? Could there be a rough-skinned newt imposter species that's evolved too? One that's all curtains & no furniture?
Here's Carl Zimmer on this arms race. Good article.
Here's another article , from PLOS, that mentions that bullfrogs also consume TTX producing newts (a different species) with apparent immunity.
Did some perusing online, and found that besides the toxic rough-skinned species, T. granulosa, there is a related species, T. torosa which is also toxic. That species is mimicked by a harmless model, Ensatina eschscholtzii. Hope I got that right.
That is very interesting! But it seems possible that the newt was not from a humongously toxic population. And if it was in the water perhaps whatever toxins it had were well diluted. Just a guess.
Just day before yesterday I saw a lovely garter snake in our forest, and yesterday a rough skinned newt! This was my first sighting of either this year- it is finally warming up I suppose.
If I recall correctly, the snake takes a hit from the poison, and begins to move very slowly. I have wondered if it is then eaten by a bird whether the TTX gets the bird too?
How lucky to witness such a thing! And have the ability to record it.
I know little of duck physiology but isn't it possible that a duck would regurgitate a poisonous meal and perhaps survive? My hope is "yes".
poor duck mustt have exploded when the newt got better.
Yikes, that was a dramatic set of photos. I had no idea newts were in danger from certain ducks. Around those parts, it would be more advantageous to be a vegetarian duck…or a filter feeder.
Great pics & subject matter, John!


No love for the PS Vita.
Adventures of Mana released today on the Google Play Store and iOS App Store. Unfortunately, the PlayStation Vita version didn't make it across the Pacific, but by all reports the mobile phone version is as feature complete as the handheld version, so at least we didn't get an inferior version.
Adventures of Mana is a remake of Final Fantasy Adventure which originally appeared on the Game Boy. The original composer, Kenji Ito, came back to compose a rearranged soundtrack, so you can be sure that there's some quality music.
You can get Adventures of Mana now on the Apple App Store or Google Play Store for $13.99.