Felicia Lo at Sweet Georgia Yarns has a Fibre Club. Once a month, for three months in a row — you get a braid of wonderfully dyed unspun fibre. It's a lovely way to experiment with new fibres and new spinning techniques.
Along with the fibre that you get with the club — approximately 4 oz — I ordered the additional amount. Which is double. My thought was that I would experiement with the first braid and then settle in with a well considered spinning approach for the second braid.
This is the February fibre. It's called "Sticky Jam". It is 75% Bluefaced Leicester and 25% Tussah Silk.
I spun this very fine on my drop spindle and plyed it on my Ashford Traditional.
This double-ply skein is about 7/8ths of a braid. So there's more to go.
The March fibre is called "Placid Waters". It is 50% merino wool, 25% bamboo and 25% tussah silk.
Felicia Lo encouraged us to maintain the richness of the colourways by Navajo plying it. The result is lovely and well advised.
The three skeins are the products of an entire braid.
The April fibre is Falkland wool and the colourway is called "Vintage Postcards". The spinning advice was for spinning a low-twist single. And the second advice is to spin slubs (a thick and thin yarn).
Haven't yet tried the slubs, but the skein shown is a low twist single. It's about 2/3rds of a braid.
That was time well spent.
So there's a lot more spinning to do as I takle the second braid in each colourway. Will try slightly different spinning techniques so I can really explore the fibre.
And of course I signed up for the next Fibre Club – May to July!
This entry was posted in fibre club, navajo plying, Sweet Georgia Yarns on April 26, 2011 by DianaTwiss.
In the midst of pulling them out of their hiding places and posing them for the photo shoots — I've been re-inspired. There are several here that I am DEFINITELY going to finish, and one that I am going to rip back and reclaim the needles.
Before you read about them, just look at the photos and see if you can guess which one is toast.
Above: This is a crocheted scarf — the yarn is amazingly soft Peruvian Cotton with a very light twist. It will make a perfect accessory to anything I own for the colours are all mine. I put it down — years ago — and everytime I pick it up, I get tripped up because I can't quite remember the pattern. I will do a row and then the feeling of — "I'm making a mistake" takes the joy out of it and I put it down.
Below is the Claudia Skirt — it's only in the unfinsihed pile because I got busy with the spinning workshops and other stuff — and I am having a hard time deciding how long I want it to be. Right now it reaches my knees. I am not sure how "inaction" is going to help me decide, but there are many things that can fill my time until I do make the decision.
Additionally, I needed a deadline to complete this and it passed. So I've created a new one for myself — the June Guild meeting — it's going to be a Celebration of our 40th Anniversary as a Guild. She will get her much overdue debut then.
This is a baby sweater. I started making it for the daughter of a girl friend — the first grandchild in our midst. I am shamed to say this little sweetie is now 5. It's all handspun yarn. I stopped knitting it because I ran out of the white yarn — had to order more fibre from the source — kid mohair and angora — spun it up, and life got in the way. It's a beauty and really deserves to be completed.
Here is the Hall of Solo Socks. Each one has its own rationalization story.
The pair below: started them with enthusiasm and designed my own pattern for it. It's a cabled leg. I was so obsessed with making the pattern that I failed to notice that you can't even see the cable work because of the variagated yarn. So I stopped. Started again half a year later when I realized that I could over-dye it an bring out the cable work. Then I lost the scrap of paper that I wrote the pattern on and I've had to read it as I go along. Not a big deal, but not a knitting pleasure.
I started making these a while ago and hated the yarn from the moment I cast on. It is a lightly twisted singles yarn. Here's a tip: If you hate the yarn at the cast on stage, you are probably going to hate it the rest of the way. And this one didn't let me down. I also dislike the length of the colour ways. It's like it's NEVER, EVER going change colour. I kept going because. . . .because I wanted to get to the red. But alas, I got out of the brown, into the green, onto the blue and then the darned GREEN and BROWN stared all over again. Trying to match these up is going to kill me. I HATE these socks.
I wrote about this pair in a blog post. I love the pattern and yarn and the needles I am using to make them. I only stopped because I had other projects to complete. I didn't want to have SSS – Second Sock Syndrome, so I made the leg of one, and then started making the leg of the other. For this pair, it's only a matter of time. I will probably bring these with me on my next trip to Winnipeg. Good knitting time on the planes.
I call these the Dirty Birthday Cake socks. The yarn has wild birthday type colours that have been muted slightly. Nothing exciting — wrote the pattern myself — like the pair above, it's only a matter of time. In fact, I started making these on my last trip to Winnipeg. Socks are good things for the plane. They pack up small and if you have the pattern memorized, you don't have to carry around a pattern book.
So there are the seven unfinished objects that I am willing at this time to share with you. The others will stay stashed until I get struck by "finish-i-tis".
Can you guess which one is going to be reclaimed? Or given away for someone else to complete?
This entry was posted in Uncategorized on April 25, 2011 by DianaTwiss.
Now that I have an accessible studio, I can waltz in there and work at my pleasure. So today, a lovely Sunday, that is exactly what I am doing. I am listening to "Cross Country Check-Up" on Radio One — of course it's about the election, and combing more of the polwarth fibre for drop spinning.
I wrote about the polwarth in a previous blog post. On all my travels this year, managed to spin up all the fibre I had prepared that weekend. It is lovely stuff — so fine and so soft. You can wear it next to your skin. There were enough combed nests to make two full spindles of finely spun singles. I wound them into hard balls and plyed them on my spindle.
It only weighs 3/4 of an ounce (20g) but it is nearly 90m of yarn. I don't know what I will do with it yet. A project hasn't called me yet. I do know that I want to dye it. Mostly because I want to see how it will take dye.
Here's the whole family of activity. The wool comb is in the top left corner with nicely combed top ready to be pulled into a roving. A couple of nests, newly made, ready for spinning are in the bottom left. My Houndesign laceweight spindle with a bit of spinning on it already. And the first skein.
Back to work and "Cross Country Check-Up".
This entry was posted in Uncategorized on April 17, 2011 by DianaTwiss.
Stuff that didn't have a place — i.e. new fibres I have brought into the house and haven't yet figured out where I am going to stash them.
Stuff that was out of its place — tools, equipment, papers, odds and sods from the demo and workshop.
So that old saying, "A place for everything and everything in its place" however irritating it may be for some to hear, is an excellent guide when tidying up a room. And here is what it looks like now. Notice the abundancy of space on the floor and clear space on table surfaces. Now there is hope that some projects can get started/worked on/completed.
I needed more space to store things, so I removed all the books from the bookshelf — filling a shelf in the hallway. Seems a little counter-intuitive to remove books from a bookshelf, but they were books, binders and reports related to my work in adult literacy. Frankly, they were taking up valuable real estate so out of the studio they went. Now that space is devoted to things I need handy, but don't want hanging around on the work tables — the lazy kate, scale, ball winder and fibre in the spinning queue.
The underside of tables are great places to store bins, boxes and sewing machines. Again, things that you want to know about — at a glance — but don't want getting in the way. The trick is to label things so you don't have to go digging about several bins to find that one bag of blue romney.
Here's the view from the doorway. Space to move around in. Supplies neatly sorted within arm's reach. Clear work tables. This is truly a space where things can happen.
This entry was posted in Uncategorized on April 16, 2011 by DianaTwiss.
I haven't done much in my studio lately, partly because I've been busy with work — travelling around, doing presentations and training events. But the real reason is because it is such a disaster I can't find my way around it. Lately I've gotten into the habit of dashing into the room to grab/find something and mostly leaving without it, 'cause I can't find it, or 'cause I can't stand being there.
I don't exactly remember when it got out of control. I think it was when I was organizing things for the Drop Spindling class I taught at FibresWest. I pulled a lot of things out of boxes and bins and reorganized them for the workshop, and never got things back to their rightful place. And then after the event itself — I scarcely had time to get in the door from that, when I was off to another town to do some literacy work. There are some boxes I still haven't unpacked from the workshop.
Then I bundled up new boxes and such for the full day demonstrations at the Bradner Flower Show last Saturday. So the mess got even more messed up.
Now I have to do something about this. What's the point of having a space to do art if you can't make your way into the room and hate being there?
Here are the boxes and such from the spinning workshop and demonstration.
Here's the other side of the room. I have somehow managed to fill every empty space with some piece of fibre in various stages of production, or a tool or piece of equipment. There's scarcely any room to actually "do art". Enough.
These will stand as "before" shots. I am going to now leave the computer and set myself to organizing this space so it is a functional studio. I will post "after" shots tomorrow.
This entry was posted in Uncategorized on April 15, 2011 by DianaTwiss.


text:
La bahía de Pensacola  es una pequeña bahía estadounidense que se encuentra en la costa del golfo de México, en la parte noroeste de la costa de Florida, una zona conocida como el panhandle de Florida.

Administrativamente, la costa de la bahía y sus aguas pertenecen a los condados de Escambia y de Santa Rosa, y es adyacente a la ciudad de Pensacola. La bahía tiene unos  de largo y 2  de ancho.

La bahía de Pensacola está formada y protegida por la península de Fairpoint y la isla de barrera de Santa Rosa, una isla de más de  que protege la bahía de los embates directos del mar, en una región que sufre frecuentes tormentas y huracanes. El puente de la bahía de Pensacola (Pensacola Bay Bridge) cruza la bahía, conectando la ciudad de Pensacola con la pequeña localidad de Gulf Breeze, localizada en el extremo occidental de la península.

La Costa Nacional Islas del Golfo (Gulf Islands National Seashore) incluye la isla de Santa Rosa, y encierra parte de la bahía. Una sección del Canal Intracostero del Golfo (Gulf Intracoastal Waterway) corre a través de la bahía. La península de Pensacola conecta con la bahía de Escambia, al norte, y con la East Bay, al este. El Pensacola Pass conecta la bahía con el golfo de México.

Historia

Primer periodo español (1559-1719)
La exploración europea de la zona comenzó en el siglo XVI. En 1516 Diego Miruelo se convirtió en el primer europeo en navegar en la bahía de Pensacola. Las expediciones de Pánfilo de Narváez en 1528 y de Hernando de Soto en 1539 visitaron la bahía, que llamaron bahía de Ochuse, relacionada con la provincia india.

El primer asentamiento español en la región fue fundado por la gran expedición de Tristán de Luna y Arellano, que desembarcó en la bahía el 15 de agosto de 1559, a la que nombró como Bahía Santa María de Filipina. Constaba la misión de más de  que llegaron en 11 barcos desde el puerto de Vera Cruz, México. Este fue el primer asentamiento europeo en el territorio de lo que hoy es Estados Unidos. Pero, semanas más tarde, la colonia fue diezmada por un huracán el 19 de septiembre de 1559, en el que murieron cientos de personas, se hundieron cinco barcos, una carabela fue arrojada a tierra firme y los suministros se arruinaron. Los  se dividieron para re ubicar/re abastecer el asentamiento, pero debido a la hambruna y a los ataques, la empresa fue abandonada en 1561. Cerca de  navegaron hasta Santa Elena (actual Parris Island, Carolina del Sur), pero otro golpe de tormenta los golpeó allí. Los sobrevivientes se dirigieron a Cuba y se dispersaron. Los restantes 50 que permanecían en Pensacola fueron llevados de vuelta a la ciudad de México, y los consejeros del virrey concluyeron que el noroeste de Florida era demasiado peligroso para asentarse. La ignoraron durante 135 años.

En 1693, el virrey mexicano Gaspar de Sandoval Silva y Mendoza, conde de Galve (1688-1696), envió al almirante Andrés de Pez para explorar la costa del Golfo, desde el norte de la bahía de Pensacola hasta la desembocadura del río Misisipi. Carlos de Sigüenza y Góngora, el reconocido mexicano científico, matemático e historiador, acompañó a De Pez. La expedición Pez-Sigüenza constaba de dos buques y partió de Veracruz a finales de marzo de 1693 llegando a Pensacola a principios de abril. Los españoles rebautizaron la bahía como Bahía Santa María de Galve (por la Virgen María y el Conde de Galve). Después de su regreso a México, Sigüenza escribió un brillante informe que respaldaba con entusiasmo el establecimiento de un asentamiento en la bahía. La Corona española aprobó el asentamiento el 13 de junio de 1694. Un año más tarde, en 1695, Andrés de Arriola inspeccionó la desembocadura del río Misisipi y la bahía de Pensacola, pero no encontró que la bahía fuese el paraíso que Sigüenza había descrito. Preocupados por la guerra del rey Guillermo (1689-1697), los españoles retrasaron la fundación hasta noviembre de 1698, bajo la dirección del ya primer gobernador, de Arriola. Construyeron tres presidios en Pensacola durante las siguientes décadas:  Presidio Santa Maria de Galve (1698–1719), el Presidio Isla de Santa Rosa (1722–1752) y el Presidio San Miguel de Panzacola (1754–1763).

La actual ciudad de Pensacola fue fundada por los españoles en 1698 como un amortiguador contra el asentamiento francés en Luisiana. San Marcos de Apalache, otro importante asentamiento español, fue establecido en 1733 en el condado de Wakulla. Los colonizadores españoles establecieron una cultura criolla en la guarnición de frontera, donde los europeos eran en su mayoría hombres, dando lugar a numerosos descendientes mestizos. Los primeros años de la colonización eran extremadamente tenue; el suelo era pobre para el cultivo de los cultivos agrícolas que se sabe que el español, y el establecimiento fue reabastecido irregular. Se consideró una publicación militar impopular debido a enfermedades tropicales, el calor, y los pobres exploradores conditions.

Los franceses fundaron Mobile en 1699, situado a unos 95 km por tierra hacia el oeste también en el golfo de México. Este asentamiento representaba la competencia y una amenaza para los españoles, que se había opuesto a los franceses en la Guerra de los Nueve Años. Los españoles también se encontraron con que los comerciantes británicos entraron en el área de la Florida desde la provincia de Carolina, para comerciar con los pueblos muskogean. Durante la Guerra de la reina Ana (1702-1713), el conflicto se dirimió en América del Norte tanto como en Europa. Los indios creek, aliados de los ingleses, hicieron repetidas incursiones en el área de Pensacola, y en 1707  sitiaron dos veces la fortaleza. Los creek, a veces junto con la milicia colonial inglesa, atacaron y dañaron severamente a los pensacolas del norte de Florida; Los supervivientes se retiraron a Pensacola, Mobile y San Agustín. Los franceses y los españoles se convirtieron en aliados contra los ingleses, y trataron de mantenerlos fuera del sudeste inferior.

Periodo francés (1719-1722)

El gobernador de la Luisiana francesa, Jean-Baptiste Le Moyne de Bienville, tomó Pensacola el 14 de mayo de 1719, llegando con su flota y una gran fuerza de tierra de guerreros indios aliados. El comandante español de Pensacola, Matamoros, no había oído que se había declarado la guerra entre Francia y España, y su guarnición era tan pequeña que él creía que sería inútil resistirse. A las cuatro de la tarde, se entregó con la condición de que los ciudadanos privados y los bienes no deben ser perturbados, y de que a la guarnición se le debía de permitir marchar con honores de guerra y ser transportada a La Habana en barcos franceses. Bienville dejó una guarnición de unos sesenta hombres en Pensacola y siguió su misión.

Los franceses, con pequeños asentamientos más al oeste en Mobile y Biloxi,  sostuvieron Pensacola durante este período. En general, las influencias francesas fueron generalmente dominante entre los criollos de la costa del Golfo al oeste de Pensacola, siendo la influencia española dominante entre los criollos en el moderno Panhandle. Un huracán expulsó a los franceses de Pensacola en 1722, que quemaron la ciudad antes de partir. Los españoles trasladaron la ciudad desde la isla de la barrera, vulnerable a las tormentas, hasta el continente.

La zona cambió muchas veces más de mano: segundo periodo español (1722-1763), Florida Occidental británica (1763-1781) y tercer periodo español (1781-1819)

Después de la guerra anglo-estadounidense de 1812, el gobierno federal decidió fortificar Pensacola y la bahía de Pensacola. Construyó el Navy Yard al oeste de la ciudad de Warrington, a partir de 1828 (este fue reconstruido en el siglo XX como Pensacola Naval Air Station). Se terminó la construcción de Fort Pickens en 1834 en el extremo occidental de la isla de Santa Rosa; Fort McRee fue completado en 1839, y el rediseño y ampliación de Fort Barrancas fue completado en 1844, a añadir a las defensas.

Derrame de petróleo en el Golfo de 2010

Tras el derrame de petróleo de Deepwater Horizon (conocido como el "derrame del Golfo"), el gobierno y British Petroleum planearon cerrar la entrada al Pensacola Pass con un sistema de barreras flotantes en junio de 2010, para controlar el flujo de la marea de petróleo que entraba desde el golfo de México. La marea alta diaria estaba haciendo que el agua contaminada con petróleo entrase en la bahía de Pensacola. Tal sistema de barrera estaba diseñado para permitir que los barcos que viajasen a través del Pensacola Pass durante la marea baja la superasen, pero que se cerraba durante la marea alta.

El plan nunca funcionó. El Paso solo se cerró un día debido a que las fuertes corrientes rompieron la barrera. Ningún otro plan se llevó a cabo en su lugar en las zonas de menos corriente ni hubo un plan para atrapar el petróleo entrante y los vertidos entraron en el Paso.

Véase también
Pensacola, Florida
Historia de Pensacola (en la Wikipedia en inglés)

Notas

Referencias

 En la Wikipedia en inglés se recogen las siguientes referencias:
The Road Atlas '06, Rand McNally, pg. 27
NOAA Nautical Charts 11382, 11383, 11384

Enlaces externos

Visit Pensacola Website

Pensacola
Pensacola
Condado de Escambia (Florida)
Condado de Santa Rosa
Pensacola (Florida)

redpajama_set_name: RedPajamaWikipedia


I did a recent (failed) experiment with waterproofing paper mache clay, so you know I've been talking a lot lately about outdoor sculptures–and especially about two previous guest posts by artists who use paper mache clay as the base, and then waterproof their sculptures with a cement product. Jackie Smith made her goddess with Thin Set mortar over the paper mache clay, and Julie Ellis made her mountain lion with Quikwall, a fiber-reinforced cement product.
This week Julie sent me photos of her latest work, and I just had to show them to you as a follow-up to her previous post. Thanks, Julie, for letting me show these to everyone.
If you want to know how she creates the sculptures, click on her link above for the full details.
They can be very heavy. The bear I'd estimate 250 pounds. The raccoons 100 pounds on the taller piece and 75 pounds on the shorter piece. That's the cement weight.
Love your work. Very nice.
Hi Julie, I need something like that for my yard, but I am afraid there might be some sticky fingers who would take them. but I will never know till I try. These are gorgeous. What do your neighbors think of your sculpture menagerie?
Christine, you bring up a good point – but maybe the weight would discourage most thieves. Julie, do you have any idea how much your sculptures weigh?
If you build it with a piece of rebar cemented in the inside of the sculpture, you can attach a short piece of chain to it. When finished, you can dig a hole where you are placing the sculpture and pour a concrete footing (wider at the bottom so it is difficult to get out) and put a piece of bent rebar in that. Once it all dries, you can lock your sculpture in place and it would take a lot of work to steal it.
Oops, never mind!! I see it now, it's the mountain lion link. Sorry!!
That's OK – I should have made it more obvious, but I was just being lazy.
I don't see the link to click on that you mentioned. I am so curious as to how she makes these! They are wonderful!


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breaking their builds and the documentation was not usable.
the C++ Now! 2014 workshop.
This one is particularly hard on the compile times.


Because the booklet of her first novel in 1992, Am?lie Nothomb keeps to interact and to impress her readers via her exploration of the fluid obstacles among good looks and monstrosity, strong and evil, delusion and truth, in addition to through her attention-grabbing presentation of formative years, anorexia, and the abject. In Am?lie Nothomb: Authorship, identification and Narrative perform, the 1st full-length learn in English of Nothomb's paintings, those parts are provided and interpreted from quite a few views, with the individuals concentrating on a unmarried novel or evaluating assorted texts. constituted of a set of essays on her autobiographical and fictional works, with contributions from her anglophone translators, it's also an interview with the writer, a preface through the eminent author and critic, Jacques de Decker and a bibliography of secondary works. Nothomb's works and the severe responses to them are contextualized in a common advent and arranged below the subsequent key issues: autobiography and gender id, representations of the physique, and narrative perform. This assortment is a vital source for college kids and students of twentieth-century modern literature and gender stories.
Jane Austen released her first novel in 1811, yet at the present time she's extra renowned than ever. movie diversifications of her books are nominated for Academy Awards. Chick lit bestsellers are in accordance with her plots. And a brand new biopic of Austen herself changing into Jane arrives in theaters this spring. For all these readers who dream approximately dwelling in Regency England, The Jane Austen guide deals step by step directions for correct comportment within the early 19th century.
CONTENTS: within the Days of the Capetian Kings well-known enthusiasts ladies in Early Provencal and French Literature girls within the Age of Saint Louis Blanche de Castille as Regent of France the mum and the spouse of a Saint The Romances of Chivalry and Love Marie de Brabant and Mahaut d'Artois Jeanne de Montfort on the courtroom of the Mad King Christine de Pisan The Savior of France The Triumph and Martyrdom of Jeanne d'Arc the increase of the Monarchy Anne de Beaujeu: The Consolidation of the dominion on the time of the unique e-book Pierce Butler, Ph.
Hèléne Cixous -- writer, playwright and French feminist theorist -- is a key determine in twentieth-century literary idea. Stigmata brings jointly her latest essays for the 1st time. Acclaimed for her complex and tough writing type, Cixous provides a set of texts that escape -- escaping the reader, the writers, the publication.
An available creation to French feminist conception and modern French women's writing for non-French audio system. The ebook deals a context to this demanding, arguable physique of labor by means of giving transparent money owed of the philosophical, post-structural and psychoanalytic debates that have had such an influence on French highbrow lifestyles lately, and to which French feminist writers supply a reaction.
Women are trapped in an existence which lies somewhere between life and death, a non-life. Once a little girl reaches puberty, Tach explains, her life has ended, and she enters into this non-life. Tach, with his cousin Léopoldine, attempts to stave off the onset of puberty through a particularly stringent regime of self-starvation in Hygiène de l'assassin, in the belief that the answer to the feminine condition is to avoid adulthood and puberty, to remain pre-adolescents. Piscina 25 They are united in an unspoken pact, and wander the grounds of the Chateau of Saint-Sulpice, isolated as if in a Garden of Eden.
The narrator's position at once inside and outside the autobiographical pact allows her to remain uncommitted to truthtelling, even to herself. She stays in that very nothingness—in the last words of Métaphysique des tubes, 'entre deux eaux' (MT 171)—she facetiously praised. From there she entertains us with her grief in coming to terms with her lost metaphysical self, lost national identity, and lost illusions concerning love. University of Western Australia Notes 1. Marthe Robert, Préface aux Contes de Grimm (Paris: Gallimard, 1990), p.
J'avais déjà fondu depuis longtemps' (MT 125). Rather than being split ('fendu') by a prescribed feminine identity, she has melted ('fondu') into her true self. The writer Amélie establishes her identity through writing ('eaux purificatrices'). The fish dreams of Métaphysique des tubes, or 'fantasmes pisciformes' (previously cited) are a motivating theme in Nothomb's writing. These fish dreams recall Hélène Cixous's 'poissonges': Plus tard si je sors de mes eaux toute ruisselante de mes plaisirs, si je remonte le long de mes rives, si j'observe depuis mon bord les ébats de mes poissonges, je remarque les figures innombrables qu'ils produisent dans leur danse; ne suffit-il pas que coulent nos eaux de femmes pour que s'écrive sans calcul nos textes sauvages et populeux?


text:
Q: BSOD crashes with no fix solution I've recently been experiencing BSOD and complete freezes for the last week. I have a custom built rig as follows:
GPU: GTX 970 Strix
CPU: Intel 2ndGen i7 2600k (1155socket sandybridge 3.4GHZ)
RAM: 16Gb razor(2 x 8GB DDR3)
MOBO: ASRock Z77 Extreme 6
PSU: Crosair CX750W
Storage: OCZ-VERTTEX4 250GB SSD & PNY CS900 120GB SSD
The first BSOD read 'IRQL_NOT_LESS_OR_EQUAL' and the next 'UNEXPECTED_KERNAL_MODE_TRAP'. From here i spoke to with Microsoft Help agents who then found a problem with my Adobe drivers. After a day the computer would then just freeze & stall with no BSOD. I was then advised to wipe my SSDs and reinstall windows but again the problem persisted. I have know been reverted back to windows update 1709 as they think my drivers for my ASrock have not yet been updated to windows 1803. They also logged a power kernal fault which indicated my PSU had critical errors just before my complete freeze today. I have looked into my PSU and the CX model is only designed for basic desktop builds whilst mines a gaming rig. This issue has only risen since the new 1803 windows updates but also as i play more render intensive games.
If anyone could shine some light on which i should try first of A. Getting a new PSU (850W Seasonic has caught my eye) or B. Buy a new MOBO as my drivers are not compatible with 1803 yet seemingly.

A: Moving the video card to a different PCIe slot solves the BSOD issues in this case. These hardware problems can be hard to detect because it doesn't always give the same error. One good way to suspect this is the problem, is that the BSOD or game crashes happen when playing graphically intense games.

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text:
package driver

import (
	context "context"

	driver "github.com/goharbor/harbor/src/pkg/quota/driver"
	mock "github.com/stretchr/testify/mock"

	types "github.com/goharbor/harbor/src/pkg/quota/types"
)

// Driver is an autogenerated mock type for the Driver type
type Driver struct {
	mock.Mock
}

// CalculateUsage provides a mock function with given fields: ctx, key
func (_m *Driver) CalculateUsage(ctx context.Context, key string) (types.ResourceList, error) {
	ret := _m.Called(ctx, key)

	var r0 types.ResourceList
	if rf, ok := ret.Get(0).(func(context.Context, string) types.ResourceList); ok {
		r0 = rf(ctx, key)
	} else {
		if ret.Get(0) != nil {
			r0 = ret.Get(0).(types.ResourceList)
		}
	}

	var r1 error
	if rf, ok := ret.Get(1).(func(context.Context, string) error); ok {
		r1 = rf(ctx, key)
	} else {
		r1 = ret.Error(1)
	}

	return r0, r1
}

// Enabled provides a mock function with given fields: ctx, key
func (_m *Driver) Enabled(ctx context.Context, key string) (bool, error) {
	ret := _m.Called(ctx, key)

	var r0 bool
	if rf, ok := ret.Get(0).(func(context.Context, string) bool); ok {
		r0 = rf(ctx, key)
	} else {
		r0 = ret.Get(0).(bool)
	}

	var r1 error
	if rf, ok := ret.Get(1).(func(context.Context, string) error); ok {
		r1 = rf(ctx, key)
	} else {
		r1 = ret.Error(1)
	}

	return r0, r1
}

// HardLimits provides a mock function with given fields: ctx
func (_m *Driver) HardLimits(ctx context.Context) types.ResourceList {
	ret := _m.Called(ctx)

	var r0 types.ResourceList
	if rf, ok := ret.Get(0).(func(context.Context) types.ResourceList); ok {
		r0 = rf(ctx)
	} else {
		if ret.Get(0) != nil {
			r0 = ret.Get(0).(types.ResourceList)
		}
	}

	return r0
}

// Load provides a mock function with given fields: ctx, key
func (_m *Driver) Load(ctx context.Context, key string) (driver.RefObject, error) {
	ret := _m.Called(ctx, key)

	var r0 driver.RefObject
	if rf, ok := ret.Get(0).(func(context.Context, string) driver.RefObject); ok {
		r0 = rf(ctx, key)
	} else {
		if ret.Get(0) != nil {
			r0 = ret.Get(0).(driver.RefObject)
		}
	}

	var r1 error
	if rf, ok := ret.Get(1).(func(context.Context, string) error); ok {
		r1 = rf(ctx, key)
	} else {
		r1 = ret.Error(1)
	}

	return r0, r1
}

// Validate provides a mock function with given fields: hardLimits
func (_m *Driver) Validate(hardLimits types.ResourceList) error {
	ret := _m.Called(hardLimits)

	var r0 error
	if rf, ok := ret.Get(0).(func(types.ResourceList) error); ok {
		r0 = rf(hardLimits)
	} else {
		r0 = ret.Error(0)
	}

	return r0
}

type mockConstructorTestingTNewDriver interface {
	mock.TestingT
	Cleanup(func())
}

// NewDriver creates a new instance of Driver. It also registers a testing interface on the mock and a cleanup function to assert the mocks expectations.
func NewDriver(t mockConstructorTestingTNewDriver) *Driver {
	mock := &Driver{}
	mock.Mock.Test(t)

	t.Cleanup(func() { mock.AssertExpectations(t) })

	return mock
}


text:
\section{Introduction}

RR Lyrae stars are of particular importance in the age and distance determination to ancient
 stellar systems, such as globular clusters. Their usefulness is based
in the fact that their light curves are easily distinguishable and  their high intrinsic
 brightness allows their detection in systems of the Local Group. Their
well defined absolute magnitude allows using them as standard candles in the cosmic distance
 scale (e.g. Alcock et al. 2004 for the LMC).

The RR Lyrae stars have been used in the determination of absolute ages of globular clusters,
 by measuring the magnitude difference between the main sequence turn
 off point and the horizontal branch (HB), on which the RR Lyrae stars reside. This is a useful
  reddening free parameter that helps in tracing the early stages of the formation of our Galaxy.
   This, however, requires a proper calibration of the absolute magnitude $M_V$ for the RR Lyraes.

The pulsational behaviour of RR Lyrae stars in globular clusters has been a subject of study for
decades since it offers insight on stellar evolution in the HB stages.
The mean periods of fundamental
pulsators (type RRab) divide globular clusters into two groups,
the Oosterhoff type I (OoI) with $<P_{ab}>$ smaller than 0.6 days and the Oosterhoff type II (OoII) with
$<P_{ab}>$ larger than 0.6 days
(Oosterhoff 1939).  Recent light curve Fourier
decomposition calculations have clearly shown that
RR Lyrae stars in OoII clusters are, on average, more luminous, more
massive and cooler than in OoI clusters, and that these quantities are closely correlated
with the mean cluster metallicity. For example these stars have longer periods in metal poor clusters
 than in metal rich clusters
 (e.g. Simon \& Clement 1993; Clement \& Shelton 1997; Kaluzny et al. 2000; Arellano Ferro et al. 2004;
Arellano Ferro et al. 2006 (see their Tables 8 and 9)).

On the other hand the period distribution of fundamental periods ($P_{ab}$ for RRab stars), and the
 fundamental periods calculated from the first overtone period and the period ratio
($P_f$ for RRc stars), as well as the relative number of RRc and RRab stars, provide important
insights relevant to the instability strip structure and HB structure and evolution (Castellani et
al. 2003). Nevertheless, such studies are strongly limited by bona fide completeness of the
sample of RR Lyrae pulsators in a cluster. It is evident from recent works that
a substantial number of RR Lyrae stars can be discovered when new image-subtraction techniques
(Alard 2000; Alard \& Lupton 1998; Bond et al. 2001; Bramich et al. 2005)
are applied to CCD images of globular clusters (e.g. Lee \& Carney 1999a; Kaluzny et al. 2001;
Clementini et al. 2004).

The latest CCD study of M2 (NGC 7089) was published by Lee \& Carney (1999a) (hereinafter LC99).
 These authors reported 13
new RR Lyraes, for a total of 34 variables in the cluster, 30 of which are RR Lyrae stars.
 They calculated the ratio
n(c)/n(ab+c) = 0.40, which
approaches the mean typical value of 0.44 in OoII clusters. Hence, not many undiscovered RR Lyraes are
expected. However, since these authors did not perform a light curve decomposition analysis,
we decided to
supplement their $BV$ data with new $VR$ observations and use the two data sets to refine the ephemerides,
 determine the mean physical parameters of the RR Lyrae stars from the Fourier decomposition
technique, compare the results with those of other similarly studied OoI and OoII clusters and,
in passing, search for new variables. The effort was not fruitless.

In Sect. 2 we describe the observations and data reductions. In Sect. 3 we calculate new
ephemerides, new times of maximum, discuss individual objects and report new variables. In Sect. 4
we calculate the physical parameters using the light curve decomposition method. In Sect. 5 we
discuss the results in the wider context of other globular clusters and in Sect. 6 we state our conclusions.

\section{Observations and Reductions}
\label{sec:Observations}

The observations used in the present work, performed using the Johnson $V$ and $R$ filters,
were obtained from June 6 to 19, 2002
with the 0.82~m telescope of the
Observatorio del Teide, Tenerife, Spain. The seeing conditions were good, with  an estimated
$FWHM \simeq 1 ~$arcsec.
The detector was a
Thompson CCD of 1024 $\times$ 1024 pixels
of 19 square microns, these images are of approximately $7 \times 7$ arcmin$^2$.
 Exposure times were 900 sec and 500 sec in the $V$ and $R$ filters,
respectively.
 A total of 60 images in $V$ and 60 in $R$ were obtained.
  Higher resolution
images for proper star identification were acquired with the 2.0 m Himalayan Chandra Telescope (HCT)
 of the Indian Astrophysical Observatory (IAO).

Differential photometry by the image subtraction method, described
in detail by Bond et al. (2001) and Bramich et al. (2005), was performed.
This procedure involves
the matching of a high quality reference image to each image in the time series,
 by solving for a spatially-varying convolution kernel and
differential sky background function. Difference images are constructed
via the subtraction of the convolved reference image from the time series
images. Photometry on the difference images yields differential fluxes for
each star relative to the flux from the reference image. Conversion of the
light curves to magnitudes requires an accurate measurement of the
reference flux.

We measured the stellar fluxes on the reference frame using DAOPhot
(Stetson 1987). However, the point-spread function (PSF) on the images was
highly non-gaussian and not fully modelled by the DAOPhot routine.
The reason for the poor PSF seems to be related with some optical
misaligment of the telescope at the time of our observations.
 Hence
our reference fluxes contain systematic errors that may
affect the amplitude
of the variable star lightcurves.
Fourier decomposition and the subsequent calculation of physical parameters
 is mainly light curve shape dependent, and
we can use our light curves for that purpose.

The instrumental magnitudes were converted to the $V$ standard system by
using 168  standard stars in the interval $19.5 > V > 14.0$ listed by Stetson (2005)
in the M2 field.
The transformation equation had a linear form
 $M_{std} = 0.985(\pm 0.005)~M_{ins} - 3.990(\pm 0.01)$, without the need of a quadratic
term; moreover, the standard stars span a $B-V$ range from $-3.5$ to $+5.0$
and no significant colour term was found.

We noticed that the difference in magnitudes between our data and LC99 light curves
changes from star to star, which is likely due
 to poor PSF quality. Then, we have shifted in magnitude each of our V light
  curves in order to match
 the LC99 photometry. Once the correct shift is applied, both data sets agree
very well, as can be seen in Fig. 1. Once the vertical matching was
accomplished we noticed a small dispersion along the time axis. Since our
 observations were gathered between 4 and 6 years after those of LC99,
   we decided to attempt a refinement of the periods, using both
data sets. The string-length method, frequency analysis and
   Fourier fits were used to detect and refine period values.
 The complete set of periods used below for the Fourier
decomposition are listed in Table 1, where the newly determined periods are
 presented alongside the periods from LC99. The differences in the periods are small
 but in several cases significant when phasing the light curves. The error on the
refined values of the periods is $2 \times 10^{-6}$ d.

In Figs. 1 and 2 the light curves in $V$ and $R$ for the previously known RR Lyraes
 are displayed.
Different symbols are used for the observations of LC99 and our own as described
in the caption, which illustrates the general good agreement between the two data sets.

\begin{figure*}
\includegraphics[width=16.cm,height=21.cm]{MARCO1.eps}
\caption{Light curves of known RRab stars in M2. They have been phased
with the new ephemerides in Table 1. The vertical scale is the same for all the stars.
Small dots represent observations from LC99. Open circles
represent observations from the present work. }
\end{figure*}

\begin{figure*}
\includegraphics[width=16.cm,height=11.cm]{MARCO2.eps}
\caption{Light curves of previously known RRc stars in M2.
Simbols are as in Fig. 1}
\end{figure*}

\begin{table}[t!]
\footnotesize{
\begin{center}
\caption[Periodos] {\small Update of periods and epochs for the RR Lyrae stars in
M2. \label{periodos} }
\hspace{0.01cm}
\begin{tabular}{lclll}
\\
\hline
\hline
Variable & Type & Old Period &  New Period   & New Epoch       \\
         &      &(days)      & (days)        & (+ 240 0000)\\
\hline
\hline
V2  & ab & 0.5278619 & 0.527840 & 52445.561 \\
V3  & ab & 0.6197084 & 0.619713 & 52445.165 \\
V4  & ab & 0.5642512 & 0.564243 & 52445.629  \\
V7  & ab & 0.5948665 & 0.594868 & 52445.347  \\
V8  & ab & 0.6437059 & 0.643690 & 52445.287 \\
V9  & ab & 0.6092938 & 0.609295 & 52445.582 \\
V10 & ab & 0.8757413 & 0.875744 & 52445.090  \\
V12 & ab & 0.6656063 & 0.665607 & 52445.248   \\
V13 & ab & 0.7066260 & 0.706619 & 52445.074   \\
V14 & ab & 0.6937767 & 0.693788 & 52445.442   \\
V15 & c  & 0.3007852 & 0.300785 & 52445.586 \\
V17 & ab & 0.6364715 & 0.636444 & 52445.474  \\
V25 & ab & 0.7287186 & 0.728720 & 52445.466  \\
V26 & c  & 0.4195213 & 0.412376 & 52445.461  \\
V27 & c  & 0.3141578 & 0.314158 & 52445.473  \\
V28 & ab & 0.8237775 & 0.823797 & 52445.210  \\
V30 & c  & 0.2728723 & 0.272871 & 52445.582  \\
V31 & ab & 0.7887144 & 0.788715 & 52445.005   \\
V32 & c  & 0.3619382 & 0.367021 & 52445.655 \\
V34 & c  & 0.3914157 & 0.391414 & 52445.639  \\
\hline
\hline
\end{tabular}
\end{center}
}
\end{table}

\section{Discussion of individual objects and new variables}

\subsection{Comments on individual variables}

For stars of steady amplitude (V3, V7, V9, V10, V12, V13, V27, V31 and V34), the agreement between the light curves of
LC99 and those in the present work is excellent. No further
discussion is needed in these cases. Other stars deserve some comments.

V2. This star is labelled as a Blazhko variable in the catalogue of Clement (2002).
 The appearance of the light curve in Fig. 1 indeed suggests that
the effect is present. The detailed plot of the light
curve displayed in Fig. 3
confirms the Blazhko nature of the variable and allows an
estimate of the magnitude variation of the maximum at different epochs (Table 2).
With only five measurements of the maximum light momenta it is difficult to characterize the
Blazhko periodicity. Nevertheless, the frequency analysis
     detected a secondary peak at 1.8870 c/d, very close to the main
     peak at 1.8945 c/d, which suggest a Blazhko periodicity of $\sim$133 d, however, the value of the secondary peak is
     not fully reliable owing to the poor phase coverage of the Blazhko cycle.

\begin{figure}
\includegraphics[width=84mm]{V2.eps}
\caption{Blazhko effect in V2.}
\end{figure}

\begin{table}
\footnotesize{
\begin{center}
\caption[Periodos y epocas] {V magnitude of maximum light variations in V2.}
\hspace{0.01cm}
\begin{tabular}{lc}
\\
\hline
\hline
$V_{max}$&HJD\\
\hline
\hline
15.532 &245 0333.667\\
15.309 &245 0358.476\\
15.374 &245 0622.921\\
15.309 &245 1057.877\\
15.878 &245 2436.609\\

\hline
\hline
\end{tabular}
\end{center}
}
\end{table}

V4, V8, V14. These stars have not been noticed before as having the Blazhko effect.
 However, the LC99 light curves show
       some cycle--to--cycle variations. Moreover, our data have
       a different amplitude in all three cases, thus, the possibility of
       a long--term Blazhko effect is just plausible, but not
       definitely proven.

V15. The light curve in our Fig. 2 and in Fig.5 of LC99, make
     the star suspected of having cycle--to--cycle variations. Since
     our analysis did not detect a radial double--mode pulsation, the
     only possibility is a Blazhko effect. Even though the time series
     has large gaps, we can tentatively explain the light curve with a
     close doublet of frequencies ($f_1$=3.3246 and $f_2$=3.2101 c/d or a
      Blazhko period of $\sim$ 8.7d).
     More observations are required to define better this doublet, since
     it seems too much separated (Moskalik \& Poretti 2003).

V17 and V25. Our light curves display a lower amplitude than in LC99, but they
    are much more accurate and rule out the possibility of a double--mode
    pulsation or a Blazhko effect. Indeed, the inspection of these stars
    on the reference image reveal that they are blends, and hence our
    amplitudes are underestimated.

V26. This star is suspected of being a double mode star in the list of Clement (2002). However
 when subdividing the data sets of LC99 and our own
into subsets, the resulting light curves look very stable although they show considerable
 time shifts ranging between 0.004~d and 0.062~d. Once the subsets are corrected by these
  shifts, a clean sinusoidal lightcurve is obtained with a period of 0.412376 days. Thus the
   star is not a double mode pulsator and the shifts can possibly be explained as light time
    effects if this RRc is a member of a binary system. More observations would be needed
to confirm this possibility.

V28. This variable seems to be rather peculiar,
 displaying a lower amplitude light curve than the other RRab stars. It is the longest
  period RR Lyrae variable in M2 (see Table 1), and its physical parameters are clearly
  discordant with those of the other RRab stars, with a particularly low
$T_{\rm eff}$  and large luminosity and radius. The possibility of an unseen blend
  affecting its light curve can not be discarded. The star could be
     an anomalous Cepheid, but its mean $V$ magnitude ($V$=15.945)
     is quite normal for an RR Lyrae variable. Owing to this peculiar behaviour,
 we didn't include its physical parameters in Tab.~6.

V30. This star is also suspected of being a double mode star in the list of Clement (2002).
 However we find it to be monoperiodic with a period of 0.272871 days. The scatter in the
  observations of both LC99 and our own is a bit large.

V32. The LC99 data show some scatter but no traces of a second periodicity have been
 found performing a frequency
      analysis. However, when splitting the time series into different
      subsets, we clearly evidenced the same light curve displaced in
      time. Therefore, a light--time effect is plausible for this star. The
       light curve displayed in Fig. 2 has been corrected of this effect.

\subsection{Negative detections}

V16. This star is reported as variable in the catalogue of
Clement (2002) and it is identified in the map of LC99.
However we find no star in the position marked by these authors nor
 variablility in nearby stars.  Therefore we have not included this star in
  Fig. 1 or in the subsequent analysis.

V18-21. These variables were not in the field of our CCD images.

V22-24. These stars, convincingly variables as reported by LC99,
were identified in our images, but no significant light variations were detected in either
the $V$ or $R$ filters despite not being in particularly crowded regions.

V29, V33. These stars are a blend in our images and the resulting
    amplitudes are very small. Our data are not useful to improve LC99
    results.

\subsection{Newly discovered variables}

We have detected clear light variations in 8 stars in the field of M2, not
previously reported as variables. The corresponding identifications are
 shown in Figs. 4 and 5.
 In Table 3, we report the period and epoch
of maximum light, and the Bailey's type for each new variable.  The error on the
 periods of the new variables is $4 \times 10^{-4}$ d.

The light curves of the new variables are shown in Fig. 6. Due to the problem with the
PSF of our images described in Sect. 2, and the fact that
these new variables are all blends to some degree (see Fig. 5), we cannot assign a
 standard magnitude for the new variables. The light curves are therefore displayed
  as differential fluxes in units of ADU/sec.
Fourier decomposition and the subsequent calculation of physical parameters
are mainly light curve shape dependent, and we can use the light curves for some of the
new variables for that purpose. The new variables are:

\begin{table}
\footnotesize{
\begin{center}
\caption[Nuevas variables] {\small Bailey's types, $(\alpha, \delta) (2000.)$
coordinates, periods and epochs for the newly detected variables. \label{nuevasvar} }
\hspace{0.01cm}
\begin{tabular}{lcllllll}
\\
\hline
\hline
Variable & Type & ~~~~$\alpha$ & ~~~$\delta$ & Period & Epoch  \\
         &      & (h ~m ~s) & ($^o$ ~$^{'}$ ~$^{"}$) & (days) & (+ 240 0000)  \\
\hline
\hline
V35  & c  & 21 33 28.0  & $-0 ~47 ~31$ &  0.32557 &  52445.517  \\
V36  & c  & 21 33 30.7  & $-0 ~49 ~12$ &  0.27078 &  52445.562  \\
V37  & ab & 21 33 26.0  & $-0 ~49 ~18$ &  0.56668 &  52445.709  \\
V38  & ab & 21 33 31.1  & $-0 ~49 ~23$ &  0.80735 &  52445.519  \\
V39  & ab & 21 33 27.3  & $-0 ~50 ~06$ &  0.60781 &  52445.467   \\
V40  & ab & 21 33 25.6  & $-0 ~49 ~15$ &  0.75173 &  52445.447  \\
V41  & ab & 21 33 28.0  & $-0 ~49 ~24$ &  0.60532 &  52445.663  \\
V42  & c  & 21 33 28.3  & $-0 ~49 ~51$ &  0.32801 &  52445.497  \\
\hline
\hline
\end{tabular}
\end{center}
}
\end{table}

\begin{figure*}
\begin{center}
\includegraphics[width=13.cm,height=10.cm]{M2AZUL.eps}
\caption{Variables in M2. Individual image stamps for the new variables
 can be found in Fig. 5. The image was obtained at the 2.0m HCT of the IAO.
  The size of the image is approximately $6 \times 6$ arcmin$^2$.}
\end{center}
\end{figure*}

\begin{figure*}
\begin{center}
\includegraphics[width=11.cm,height=11.cm]{COMPOSITION.eps}
\caption{Detailed identifications of new variables in M2. The size of the
 stamps is 17 $\times$ 17 arc seconds. As in Fig. 4 north is down and east is to the right.}
\end{center}
\end{figure*}

V35. This RRc variable appears in the V images as a blend with another
brighter
star by about two magnitudes, and it is not detected in the R images.
 This star will not be considered for physical parameter calculations.

V36 and V42. These are new RRc variables.

V37, V38, V39, and V40. These stars show clear light curves of the RRab type.
V37 is not detected in the R images.

V41. This is a strong blend not resolved in our images. The variability in
the difference images has a small offset relative to the centre of the
contaminating brighter star. The variable is of type RRab.

\begin{figure*}
\includegraphics[width=16.cm,height=11.cm]{MARCO3flux.eps}
\caption{Light curves of the new variables. For identifications refer
to Figs. 5 and 6. The vertical scales are  differential fluxes in ADU/sec. Thus the amplitudes
are artificial and not comparable between different filters and stars.}
\end{figure*}

\section{Fourier light curves decomposition and physical parameters}

 The mathematical representation of the light curves is of the  form:

\begin{equation}
m(t) = A_o ~+~ \sum_{k=1}^{N}{A_k ~cos~( {2\pi \over P}~k~(t-E) ~+~ \phi_k ) }
\end{equation}

\noindent
where $m(t)$ are magnitudes at time $t$, $P$ the period and $E$ the epoch. A linear
minimization routine is used to fit the data with the Fourier series model, deriving
the best fit values of $E$ and of the amplitudes $A_k$ and phases $\phi_k$ of
 the sinusoidal components.

The fits are not shown in Figs. 1, 2 and 6 for simplicity and clarity.
From the amplitudes and phases of the harmonics in eq. 1, the Fourier parameters,
defined as $\phi_{ij} = j\phi_{i} - i\phi_{j}$, and $R_{ij} = A_{i}/A_{j}$,
were calculated.
The mean magnitudes $A_0$, and the Fourier light curve fitting parameters of the individual RRab and
 RRc type stars in
$V$ are listed in Table 4. The mean dispersion about the fits is about  $\pm 0.022$ mag.
These parameters will be used below to estimate the physical parameters of the stars.

The realization that light curve shapes and physical parameters are related, traces back to the
paper of Walraven (1953). The relation between the pulsation of RR Lyrae variables and
their physical parameters is obtained from hydrodynamic pulsation models of defined physical parameters,
 which are used to generate theoretical light curves. These curves are then fitted to obtain
the corresponding Fourier parameters. Simon \& Clement (1993) used
 hydrodynamic pulsation models to calibrate equations for the effective temperature $T_{\rm eff}$,
 a helium content parameter $Y$,
the stellar mass $M$ and the luminosity $L$, in terms of the period and Fourier parameter
$\phi_{31}$ for RR Lyrae stars of the Bailey's type RRc (see eqs. 2, 3, 4 and 5).
Recently, Morgan {\it et al.} (2005) have found several [Fe/H] - log~P - $\phi_{31}$ relations for
RRc variables, and we have adopted their eq. 5 (see eq. 6 below), with a quoted
standard deviation of $\pm 0.21$, to
derive the [Fe/H] values given in Table 5. $M_V$ for the RRc stars can be estimated
 through the calibration given by Kov\'acs (1998) (eq. 7). For the sake of clarity, all the equations
  used are listed below:

\begin{equation}
log~M/M_\odot = 0.52~log~P ~-~ 0.11~\phi^{(c)}_{31} ~+~ 0.39
\end{equation}

\begin{equation}
	log~L/L_\odot = 1.04~log~P - 0.058~\phi^{(c)}_{31} ~+~ 2.41
\end{equation}

\begin{equation}
	log T_{\rm eff} = 3.775 ~-~ 0.1452~log~P ~+~ 0.0056~\phi^{(c)}_{31}
\end{equation}
$$	log~Y = -20.26 ~+~ 4.935~log~T_{\rm eff} ~-~ 0.2638~log~M/M_\odot ~+~ $$
\begin{equation}
~~~~~~~	~+~ 0.3318~log~L/L_\odot
\end{equation}
$$ [Fe/H] = 3.702~(log~P)^2 ~+~ 0.124~(\phi^{(c)}_{31})^2 ~-~ 0.845~\phi^{(c)}_{31} ~-~ $$
\begin{equation}
~~~~~~~	~-~ 1.023~\phi^{(c)}_{31}~log~P ~-~ 2.620
\end{equation}
\begin{equation}
M_V = 1.261 ~-~ 0.961~P ~-~ 0.044~\phi^{(s)}_{21} ~-~ 4.447~A_4
\end{equation}

For the RRab stars we have used the eq. 3 of Jurcsik \& Kov\'acs (1996) for [Fe/H] (our eq. 8),
eq. 2 in Kov\'acs \& Jurcsik (1996) for $M_V$ (our eq. 9), and eqs. 5 and 11 in Jurcsik (1998)
for $(V - K)_o$ and log $T_{\rm eff}$ (our eqs. 10 and 11). The explicit formulae are:

\begin{equation}
	[Fe/H] = -5.038 ~-~ 5.394~P ~+~ 1.345~\phi^{(s)}_{31}
\end{equation}
\begin{equation}
	M_V= 1.221 ~-~ 1.396~P ~-~ 0.477~A_1 ~+~ 0.103~\phi^{(s)}_{31}
\end{equation}
$$ (V - K)_o= 1.585 ~+~ 1.257~P ~-~ 0.273~A_1 ~-~ 0.234~\phi^{(s)}_{31} ~+~ $$
\begin{equation}
~~~~~~~ ~+~ 0.062~\phi^{(s)}_{41}
\end{equation}
\begin{equation}
	log~T_{\rm eff}= 3.9291 ~-~ 0.1112~(V - K)_o ~-~ 0.0032~[Fe/H] ~~~~
\end{equation}

The luminosity is derived through $M_V$ and the bolometric correction $BC$,
 adopting the relation of Sandage \& Cacciari (1990):
\begin{equation}
 BC = 0.06~[Fe/H] ~+~ 0.06
\end{equation}
With:
\begin{equation}
M_{bol} = M_V ~+~ BC ~~~~ {\rm and} ~~~~ log~L/L_\odot= -0.4 ~( M_{bol} ~-~ 4.75 ) ~~~~
\end{equation}

In the previous equations, $\phi^{(c)}_{jk}$ and $\phi^{(s)}_{jk}$ are phase shifts with
assumed cosines and sines Fourier series respectively, they are related by:
  ~~ $\phi^{(s)}_{jk} = \phi^{(c)}_{jk} - (j - k) {\pi \over 2}$.\\

A thorough discussion of the uncertainties in the physical parameters, as obtained
from the above mentioned calibrations,
can be found in the work of Jurcsik (1998). The estimated uncertainties
for log~$L$, log $T$, log $M$ and [Fe/H] are  $\pm 0.009, \pm 0.003, \pm0.026$ and $\pm 0.14$ dex
respectively.

We have carried out the Fourier decomposition of RRab stars using the combined data of
LC99 and our own, except in those stars where the Blazhko effect is confirmed
or suspected, i.e. in V2, V4, V8, V14 and V15.
 Moreover, V31, V40 and V41 data are less reliable owing to high scatter and/or gaps in the
   phase coverage: also these
 stars have been not considered. Tables 5 and 6 list the physical parameters we
  obtained.

  We notice that the average value of [Fe/H] we
derived from our RRab sample ($-1.47$)
is in close agreement with  that
reported by Kovacs \& Walker (2001; [Fe/H]=$-1.43\pm0.15$). Also when
including the two RRc stars (as Kovacs \& Walker did),
the average value ([Fe/H]=$-1.50 \pm 0.17$) is within the error bars.

It must be noticed that $M_V$ derived from eqs. 7 and 9 for RRc and RRab stars respectively,
 agree very well. However the luminosities
for RRc stars derived from eq. 3 seem to be too large when compared with those for
RRab variables (derived from eqs. 9, 12 and 13). This can be appreciated in Fig. 8
 (open circles and crosses).
The possibility that this is the result of the temperature dependence of the bolometric correction, $BC$,
 can be ruled out as it does not explain the difference in $log~L/L_\odot$. Alternatively, if eq. 12
  is used to transform the $M_V$ values, obtained with eq. 7, into $log~L/L_\odot$, both RRc and RRab
   stars have similar luminosities (crosses in Fig. 8). Moreover, the $A_0$ values
    of the  RRc  stars reported in Table~4~(V27, V30, V32 and V34) are quite similar
     to those of the RRab stars.
 Then, some inconsistency seems to exists between the zero points of eq. 3 and eq. 7
 for the RRc stars. This problem has been noticed and commented by Cacciari et al. (2005)
   whom opted for decreasing the magnitud scale derived from eq. 7 by 0.20 mag.

\begin{table}
\footnotesize{
\begin{center}
\caption[Fourier fitting parameters for V light curves] {\small Fourier
fitting parameters for V light curves}
\hspace{0.001cm}
\begin{tabular}{lcccccc}
\\
\hline
\hline
Star (N)&$A_0$&$A_1$&$A_4$&$\phi_{21}$&$\phi_{31}$&$\phi_{41}$\\
\hline
\hline
V3 (9)&16.007&0.362&0.084&4.03&2.05&0.17\\
V7 (8)&15.995&0.391&0.084&3.95&1.91&6.14\\
V9 (8)&16.038&0.356&0.077&3.98&1.99&0.10\\
V10 (8)&15.753&0.246&0.019&4.48&3.06&1.27\\
V12 (8)&15.957&0.349&0.075&4.17&2.29&0.64\\
V13 (6)&15.952&0.275&0.045&4.19&2.33&0.61\\
V17 (8)&16.056&0.196&0.052&3.89&1.72&5.98\\
V25 (5)&16.211&0.118&0.011&4.03&2.18&0.26\\
V27 (1)&15.954&0.047& & & &\\
V28 (2)&15.945&0.079& &4.79&   &\\
V30 (1)&16.126&0.079&   &   &   & \\
V31 (4)&16.074&0.184&0.013&4.48&3.06&1.66\\
V32 (4)&16.085&0.201&0.005&4.66&3.50&2.70\\
V34 (4)&15.983&0.213&0.013&5.38&4.50&3.23\\
V36 (2)&--&0.077& &4.36& & \\
V37 (7)&--&0.123&0.040&3.61&1.51&5.59\\
V38 (4)&--&0.107&0.008&4.39&2.63&0.89\\
V39 (6)&--&0.097&0.017&3.96&2.09&6.10\\
V41 (4)&--&0.048&0.014&4.03&2.31&0.06\\
\hline
$\langle\sigma_{RRab}\rangle$&$\pm$0.002&$\pm$0.003&$\pm$0.003&$\pm$0.07&$\pm$0.11&$\pm$0.18\\
$\langle\sigma_{RRc}\rangle$&$\pm$0.002&$\pm$0.004&$\pm$0.004&$\pm$0.24&$\pm$0.37&$\pm$0.66\\
\hline
\hline
\end{tabular}
\end{center}
N: number of harmonics used to fit the light curve.\\
$A_0$ : after shifting our data to fit the LC99 magnitude scale.\\
V17 and V25 : light curve fitting on our data only.
}
\end{table}

\section{Discussion}

\subsection{Oosterhoff type and RR Lyrae statistics}

Including the 3 new variables the average value of the period for the RRc stars is 0.327 $\pm$ 0.044 days.
 Comparing with the mean values for seven clusters
reported by Clement \& Rowe (1999), M2 fits better among the OoI type, although considering the
 standard deviations, the difference from the value in OoII type clusters of 0.36 days, is not
  significant.
For the RRab stars, including the 5 new variables, we find an average period of 0.674
 $\pm$0.093 days which is typical of Oo II type clusters (average ~0.65 days). Therefore,
  it seems that M2 is a borderline case between OoI and OoII type clusters.

\begin{table*}
\footnotesize{
\begin{center}
\caption[Parametros estelares de las RR Lyrae del tipo  c] {\small  Physical parameters for the
RR{\lowercase {c}} stars   \label{parametrosc} }
\hspace{0.01cm}
\begin{tabular}{lccccccccc}
\\
\hline
\hline
Star & [Fe/H] & $T_{\rm eff}$ & $M_V$ & $log (L/L_\odot)$ & $Y$ & $M/M_\odot$ &
 $log (R/R_\odot)$ (LT) & $log (R/R_\odot)$ (PRZ) & D ($kpc.$) \\
\noalign{\smallskip}
\hline
\hline
\noalign{\smallskip}
V32 & $-1.798$ & 7202. &  0.75 & 1.754 &  0.26 &  0.60 &  0.713 &  0.710 &  10.71 ~~~~ \\
V34 & $-1.422$ & 7228. &  0.66 & 1.725 &  0.28 &  0.48 &  0.673 &  0.728 &  10.64 ~~~~ \\
\hline
Mean  &$-1.61$ & 7215. &  0.71 &  1.74 &  0.27 &  0.54 &  0.69 &  0.68 &  10.67 \\
$\sigma$ &  $\pm$ 0.27 & $\pm$ 18.& $\pm$ 0.06& $\pm$ 0.02 & $\pm$ 0.01 & $\pm$ 0.08 &
$\pm$ 0.03 & $\pm$ 0.04 & $\pm$  0.05 \\
\noalign{\smallskip}
\hline
\hline
\end{tabular}
\end{center}
}
\end{table*}

\begin{table*}
\footnotesize{
\begin{center}
\caption[Parametros estelares de las RR Lyrae del tipo ab] {\small Physical parameters for the RR{\lowercase {ab}}
  stars \label{parametrosab} }
\hspace{0.01cm}
\begin{tabular}{lccccccc}
\\
\hline
\hline
Star  & [Fe/H] & $T_{\rm eff}$ & $M_V$  & $log (L/L_\odot)$ &  $log (R/R_\odot)$ (LT) &
 $log (R/R_\odot)$ (PRZ) & D ($kpc.$) \\
\noalign{\smallskip}
\hline
\hline
\noalign{\smallskip}
V3   & $-1.398$ & 6380. &  0.72 &  1.622 &  0.729 &  0.767 &  10.49 \\
V7   & $-1.452$ & 6424. &  0.72 &  1.621 &  0.720 &  0.756 &  10.40 \\
V9   & $-1.421$ & 6384. &  0.73 &  1.618 &  0.727 &  0.762 &  10.58 \\
V10  & $-1.421$ & 6084. &  0.52 &  1.702 &  0.808 &  0.854 &  10.22 \\
V12  & $-1.323$ & 6320. &  0.68 &  1.634 &  0.744 &  0.785 &  10.40 \\
V13  & $-1.490$ & 6231. &  0.67 &  1.645 &  0.758 &  0.800 &  10.47 \\
V37  & $-1.824$ & 6287. &  0.85 &  1.579 &  0.714 &  0.744 &   ~-~ \\
V38  & $-1.630$ & 6049. &  0.64 &  1.660 &  0.790 &  0.833 &   ~-~ \\
V39  & $-1.280$ & 6331. &  0.87 &  1.561 &  0.705 &  0.762 &   ~-~ \\
\hline
Mean & $-1.47$ &  6276. &  0.71 &  1.63 &  0.75 &  0.79 &  10.42 \\
$\sigma$ & $\pm$ 0.16 &  $\pm$ 124. & $\pm$ 0.10& $\pm$ 0.04& $\pm$ 0.03& $\pm$ 0.04& $\pm$0.11 \\
\noalign{\smallskip}
\hline
\hline
\end{tabular}
\end{center}
}
\end{table*}

After LC99 reported 13 new RR Lyraes, for a total of 30 in the cluster, the ratio
n(c)/n(ab+c) = 0.40
approached the mean typical value of 0.44 in OoII clusters and argued that not many undiscovered RR Lyraes
are expected. We have found 8 new variables and a new value n(c)/n(ab+c) = 0.41
 (negative detections excluded as variables ).
We see no reason for not finding yet more RR Lyraes in this cluster if adequate monitoring is performed.

\subsection{RR Lyrae radii}

Given $log(L/L_\odot)$ ($M_V$ for RRab) and $T_{\rm eff}$ in Tables 5 and 6 one can derive the stellar radii.
These radii depend fully on the semi-empirical relations and the hydrodynamical models used to calculate the
 luminosity and temperature, and they are included in Tables 5 and 6 under the name $log (R/R_{\odot}) (LT)$.
  Recently
Marconi {\it et al.} (2005) have offered Period-Radius-Metallicity (PRZ) relationships for the RR Lyrae
based on the nonlinear convective models of Bono et al. (2003 and references therein). In these
relations the mean radius can be obtained from the pulsation period and the metallicity parameter $Z$.
We have used these calibrations to calculate the radii of the RR Lyrae in M2
and compare them with the radii obtained independently from the light curve Fourier decomposition.
 In doing so, we have converted the [Fe/H] parameter
into Z making use of the equation:
$log~\rm{Z} = \rm{[Fe/H]} - 1.70 + log (0.638~f + 0.362)$ where $f$ is the
 $\alpha$-enhancement factor with respect to iron (Salaris et al. 1993) which we adopt as
  $f=1$. The radius can be estimated using the individual values of [Fe/H] in Table 6
or the average value $-1.543$. We have found that the differences in the estimated radii
are not significant. Thus we report in Tables 5 and 6 the radii
from P and Z, labelled  $log (R/R_{\odot})$ (PRZ) using the average [Fe/H].

\begin{figure}
\includegraphics[width=6.cm,height=8.cm, angle=-90.]{FIG7.eps}
\caption{Comparison of radii from the Fourier decomposition parameters $L$ and $T_{\rm eff}$
with those obtained from the Marconi {\it et al.} (2005) calibration from $P$ and $Z$.
 Solid circles represent RRab stars and open circles RRc stars}
\end{figure}

In Fig. 7 the comparison of $log (R/R_{\odot})$ (LT) and $log (R/R_{\odot})$ (PRZ)
is shown. As seen in Tables 5 and 6, and Fig. 7, the $log (R/R_{\odot})$
 (PRZ) values are systematically larger than $log (R/R_{\odot})$ (LT) by about 0.04.
But given that both radii determinations are based on different models,
methods and calibrations, and the sensitivity of radii to the opacity and
other ingredients in the stellar models, both determinations can be considered quite
consistent.

\subsection{Distance to M2}

To calculate the distance to the cluster we have calculated the distance moduli $(A_0 - M_V)$
 for each star, using the absolute magnitudes
$M_V$, given in Tables 5 and 6, derived from the Fourier parameters listed in Table 4.
The total to selective extinction ratio $R= A_V/E(B - V)= 3.1$, with $E(B - V)= 0.06$ (Harris 1996),
was adopted to correct for interstellar extinction.
For the RRab stars the $M_V$ values were obtained from the calibration of
 Kov\'acs \& Jurcsik (1996),
while for the RRc stars the relation of Kovacs (1998) was used to derive $M_V$.

We find a mean distance of $10.42 \pm 0.12$ kpc for the RRab and
$10.67 \pm 0.05$ kpc for the RRc stars respectively.
The uncertainty in these values is the standard deviation of the mean from individual stars.
Our mean value of the distance to M2, $10.49 \pm 0.15$ kpc,
 from eleven RRab and RRc variables, is to be compared with the  previous estimates of
 11.5 and 11.2 kpc reported by Harris (1975; 1996), respectively.

\subsection{On the evolutionary stage of the RR Lyrae stars}

From the values in Tables 5 and 6 we can place the
RRc and RRab stars in the  HR diagram in Fig. 8.
Two versions of the instability strip are shown.
    The vertical boundaries are the fundamental (continuous lines) and first overtone
    (dashed lines) instability strips from Bono et al. (1995), $M= 0.65 ~M_{\odot}$,
     Y= 0.24 and Z= 0.001 .
  As shown in the figure, the RRab variables populate the fundamental mode band
  in a narrow region in $T_{\rm eff}$ near the red edge of the theoretical instability
  strip, whereas the two RRc stars are located close to the first overtone blue edge.
  The small number of RRc variables in our diagram does not allow to discuss
   the suggestion of Bono et al. (1995) that in OoII clusters the
   transition between RRc and RRab variability occurs near the first overtone
    red edge, while in the OoI clusters the transition is found closer to the
    fundamental blue edge.
          The short continuous tilted lines are the empirical
   fundamental mode instability strip found by Jurcsik (1998) from 272 RRab stars
    of different metallicity, including variables from galactic field stars,
   many globular clusters and the Sculptor dwarf galaxy.
  It seems rather surprising that the empirical instability band is much narrower
  that the modelled one from Bono et al. (1995), even if it is defined from a
  very inhomogeneous sample of RRab variables. It is also clear that the location
   of the RRab stars in M2 follows closely the empirical strip both in slope and width.

Two values for the luminosity of the two RRc stars are plotted in Fig. 8. The upper
 values, open circles, correspond to the values obtained from eq. 3.
The lower values are those obtained from the Mv values from eq. 7 and transformed
 into luminosity by the eqs. 12 and 13. While the apparent and absolute magnitudes
 of the RRc stars agree with those of the RRab stars, it is clear that the luminosity
predicted from eq. 3 is large. We shall retain these large values for further
 comparison, in section 5.5, with RRc stars
in other globular clusters studied by the Fourier decomposition technique.

The theoretical zero age horizontal branch (ZAHB) from the RRab models of Lee \& Demarque (1990)
 for two chemical mixtures,
 (Y=0.20;Z=0.0001) and (Y=0.23; Z=0.0007) are also shown in Fig. 8. These
  two ZAHB`s lie above the RRab stars. However,
  the estimated value of the relative abundance of helium for our RRc sample is Y=0.27, for
   which a model is not available. Since the luminosity of the ZAHB decreases with increasing Y,
    an extrapolation of Lee \& Demarque (1990) models to larger values of Y would make the
     ZAHB match the distribution of RRab stars.

\begin{figure}
\includegraphics[width=84mm]{FIG8.eps}
\caption{Solid circles represent RRab stars, open circles RRc stars with $log(L/L_\odot)$
 calculated from eq. 3 and crosses RRc stars with $log(L/L_\odot)$ calculated from $M_V$.
The solid tilted lines indicate the empirical bounds found by Jurcsic (1998)
from 272 RRab stars. The vertical boundaries are the fundamental
(continuum lines) and first overtone (dashed lines) instability strips from
Bono et al. (1995) for 0.65 $M/M_\odot$.
Two models of the ZAHB (Lee \& Demarque 1990) are shown and
labelled with the corresponding metallicities. An extrapolation of these models to the value
of $Y=0.27$ (found from the RRc stars) would place the RRab stars near the ZAHB.}
\end{figure}

\subsection{Physical parameter trends in globular clusters}

The mean parameters for the RRc and RRab stars are compared for several clusters in Tables 7 and 8.
 These tables contain only those clusters for which their mean parameters have been obtained from
  the technique of RR Lyrae
light curve Fourier decomposition and are updated versions of equivalent tables previously published
 by Arellano Ferro et al. (2004; 2006) and Kaluzny et al. (2000).

\begin{table*}
\begin{center}
\caption[Parametros RRc] {\small Mean
physical parameters obtained from RR{\lowercase {c}} stars in globular clusters.}
\hspace{0.01cm}
\begin{tabular}{cccccccc}
\\
\hline
\hline
Cluster  & Oo type & [Fe/H] & No. of stars& $M/M_\odot$ &  $log(L/L_\odot)$ &  $T_{\rm eff}$ & $Y$ \\
\noalign{\smallskip}
\hline
\hline
\noalign{\smallskip}
NGC~6171 & I & $-0.68$& 6&0.53 &1.65 &7447&0.29 \\
NGC~4147$^1$& I &$-1.22$&9&0.55 & 1.693 & 7335& 0.28 \\
M5      &I  & $-1.25$& 7&0.58 & 1.68 &7338&0.28\\
M5$^2$      &I  &$ -1.25$&14&0.54 & 1.69 &7353&0.28\\
M3$^3$      &I  &$-1.47$& 5&0.59& 1.71 & 7315&0.27\\
NGC 6934$^4$&I  &$-1.53$& 4&0.63& 1.72 & 7300&0.27\\
{\bf M2$^5$}  & II & $-1.61$ & 2 & 0.54 & 1.739 & 7215  & 0.27\\
M9      &II&$-1.72$&1& 0.60&1.72  & 7299&0.27\\
M55$^6$ &II&$-1.90$&5&0.53& 1.75&  7193&  0.27\\
NGC~2298 &II&$-1.90$&2&0.59&1.75& 7200&0.26\\
M92$^7$ & II &$-1.87$&3&0.64&1.77&7186&0.26\\
M68    &II&$-2.03$&16&0.70&1.79&7145& 0.25\\
M15   & II&$-2.28$&6& 0.73&1.80&7136&0.25\\
M15$^8$ & II &$-2.12$&8& 0.76 & 1.81 & 7112 & 0.24\\
\noalign{\smallskip}
\hline
\hline
\end{tabular}
\end{center}
Data taken from Clement \& Shelton (1997), except:\\
1. Arellano Ferro {\it et al.} (2004), 2. Kaluzny {\it et al.} (2000),
 3. Kaluzny {\it et al.} (1998), 4. Kaluzny et al. (2001),
5. This work, 6. Olech {\it et al.} (1999),
 7. recalculated in this work from the data of Mar\1n (2002), 8. Arellano Ferro {\it et al.} (2006).
\end{table*}

\begin{table*}
\begin{center}
\caption[Parametros RRab] {\small Mean
physical parameters obtained from RR{\lowercase {ab}} stars in globular clusters.}\label{kaluznyab}
\hspace{0.01cm}
\begin{tabular}{cccccc}
\\
\hline
\hline
Cluster  & Oo type&No. of stars & [Fe/H]  &  $T_{\rm eff}$ & $M_V$\\
\noalign{\smallskip}
\hline
\hline
\noalign{\smallskip}
NGC~6171$^1$ & I  &3& $-0.91$ &6619&0.85   \\
NGC~4147$^2$& I  &5& $-1.22$ &6633&0.80   \\
NGC1851$^3$ & I  &7&$-1.22$  &6494&0.80    \\
M5$^4$       & I  &26&$-1.23$ & 6465&0.81  \\
M3$^5$       & I  &17&$-1.42$ & 6438&0.78  \\
NGC 6934$^6$& I& 24&$-1.53$& 6450&0.81 \\
M55$^7$  & II &5&$-1.48$ & 6352&0.71  \\
{\bf M2$^8$}& II & 9 & $-1.47$ & 6276 & 0.71  \\
M92$^9$  & II &5&$-1.87$ & 6160&0.67 \\
M15$^{10}$  & II &11&$-1.87$ & 6237&0.67 \\
\noalign{\smallskip}
\noalign{\smallskip}
\hline
\hline
\end{tabular}
\end{center}
1. Clement \& Shelton (1997), 2. Arellano Ferro {\it et al.} (2004), 3. Walker (1999),
 4. Kaluzny {\it et al.} (2000), 5. Kaluzny {\it et al.} (1998), 6. Kaluzny et al. (2001), 7. Olech {\it et al.} (1999), 8. This work,
  9. recalculated in this work from the data of Mar\1n (2002),
 10. Arellano Ferro {\it et al.} (2006).
\end{table*}

\begin{figure}
\includegraphics[width=84mm,height=9.cm]{FIG9.eps}
\caption{General trends of relevant physical parameters in globular clusters
as a function of metallicity. All these parameters have been calculated by
the RRc stars light curve Fourier decomposition technique. The error bars are the standard deviation of the
 mean divided by the square root of the number of stars included in each cluster. The horizontal error bar
  in the metallicity is a mean
uncertainty calculated using the expression from Jurcsik \& Kov\'acs (1996), their eq. 4.
 Error bars have only been calculated for those clusters studied by our team. Label dot has not been included in the fit.}
\end{figure}

\begin{figure}
\includegraphics[width=84mm,height=6.cm]{FIG10.eps}
\caption{Same as Fig. 9 but for the RRab stars. The dashed line corresponds to eq. 19.
 This indicates that eq. 3 makes the RRc stars to appear brighter than RRab stars by about 0.20 mag. See text in section 4 for discussion.}
\end{figure}

Figs. 9 and 10 show the trends of physical parameters as a function of metallicity
for RRc and RRab stars respectively. The dependences on metallicity are clear in all cases,
especially for $log L/L_{\odot}$ and $T_{\rm eff}$. The straight lines in the figures are the least square
  fits to the point distribution. The relationships representing the lines are:\\

For the RRc stars:

\begin{equation}
log~M/M_{\odot} = - ( 0.105 \pm 0.019 )~\rm{[Fe/H]} - ( 0.381 \pm 0.032 )
\end{equation}
\begin{equation}
log~L/L_{\odot} = - ( 0.111 \pm 0.009 )~\rm{[Fe/H]} + ( 1.554 \pm 0.016 )
\end{equation}
\begin{equation}
log~T_{\rm eff} = + ( 0.013 \pm 0.001 )~\rm{[Fe/H]} + ( 3.882 \pm 0.002 )
\end{equation}

The uncertainties in $log M/M_{\odot}$, $log L/L_{\odot}$, and $log T_{\rm eff}$  in the above calibrations are:
 0.029, 0.014, and 0.002 respectively.\\

For the RRab stars:
\begin{equation}
log~T_{\rm eff} = + ( 0.032 \pm 0.006 )~\rm{[Fe/H]}  + ( 3.852 \pm 0.008 )
\end{equation}
\begin{equation}
M_V~= + ( 0.191 \pm 0.037 )~\rm{[Fe/H]} + ( 1.032 \pm 0.054 )
\end{equation}

The uncertainties in $log T_{\rm eff}$ and $M_V$ are 0.004 and 0.031 respectively.

 The relationship between $log L/L_{\odot}$ and [Fe/H] for the RRc stars (eq. 15)
is very tight, and can be transformed into a $M_V$ - [Fe/H] relationship with the
bolometric correction. Adopting the $BC - \rm{[Fe/H]}$ relation of Sandage \& Cacciari (1990) and
 $M_{bol,\odot}= 4.75$, we derive the relation:

\begin{equation}
 M_V= + ( 0.22 \pm 0.03 ) ~{\rm [Fe/H]} ~+~ ( 0.86 \pm 0.05 )
\end{equation}

This relation, shown as a dashed line in the lower panel of Fig. 10,
has a small zero point difference with
the average relationship obtained from several methods by Chaboyer (1999):
  ~$M_V = ( 0.23 \pm 0.04 )~\rm{[Fe/H]} ~+~ ( 0.93 \pm 0.12 )$.
Eq. 19 can be used to estimate an average $M_V= 0.53 \pm 0.08$ at
 [Fe/H] =$-$1.50. This result is in good agreement with the
weighted average of $M_V = 0.58 \pm 0.04$ obtained by Cacciari (2003) from various
 methods, or with the weighted average of seven clusters obtained by Chaboyer (1999)
  $M_V = 0.61 \pm 0.11$, both for $\rm{[Fe/H]} = -1.50$.
Thus, the zero point predicted by the luminosities of eq. 3 (Simon \& Clement 1993)
 is in agreement with the above independent estimates, but it is
 about 0.20 mag. too bright relative to the zero point predicted by the calibrations
  of eqs. 7 and 9 for the RRc and RRab stars (Kov\'acs 1998;
   Kov\'acs \& Jurcsic 1996).

We do not find the discontinuity in the  $M_V$ $-$ [Fe/H] relation claimed by
 Lee \& Carney (1999b) but find rather a smooth transition between OoI and OoII clusters.\\

The above equations represent general laws for the horizontal branch position and structure
 as a function of metallicity and seem to hold for globular clusters at  a wide range
  of galactocentric distances and metallicities.

The trends given by eqs. (15), (18), and (19) agree with previous studies in that
 the RR Lyrae variables are more luminous (hence more evolved) in lower metalicity (hence older) clusters.

The relationship between $M_V$ and [Fe/H] has been widely discussed in the literature.
 Some evidence of the non linearity of the $M_V$ $-$ [Fe/H] relationship has been offered
 from empirical (Caputo et al. 2000; Demarque et al. 2000) and theoretical arguments
(Cassisi et al. 1999; Ferraro et al. 1999; VandenBerg et al. 2000).

Of particular interest is the $log M/M_{\odot}$ vs. [Fe/H] relation for the RRc variables.
 It is evident that RRc
 stars in OoII clusters have systematically larger masses than in OoI clusters.
However, Clement \& Rowe (2000), in a study of RRc variables in the clusters $\omega$~Cen, M55 and M3
 reached the opposite conclusion. They found an increase of the mass with luminosity
 within each of the Oosterhoff groups, but a discontinuity at the transition
 between the OoI and OoII clusters. They derived lower masses and higher luminosities
  for the OoII RRc variables in $\omega$~Cen and M55 than the OoI RRc variables in $\omega$~Cen and M3,
 and a similar behaviour for the RRab variables. It seems that this conclusion could have been
 strongly influenced by the low value of $log M/M_{\odot}$ for the cluster M55. However,
  our Figs. 9 and 10 (see also Tables 7 and 8), based on a larger number of clusters, suggest
 a continuous trend with metallicity, and do not support any significant discontinuity between
 OoI and OoII variables.

The trends in Figs. 9 and 10 and the related equations support the general scheme that
 OoII clusters are older and less metallic than OoI clusters, with their RR Lyrae
  being more massive, more luminous and having longer periods. This would be
expected if the mass loss at the tip of the Red Giant Branch is diminished for smaller
metallicities; thus in older clusters, at the time of reaching the HB stage, the stars turn into
 slightly more massive RR Lyrae
variables with lower $T_{\rm eff}$ but larger luminosity,
as expected from models of HB stars.
 This is consistent with the hypothesis that the origin of the
Oosterhoff dichotomy is age; in OoII the stars are more massive, older and more evolved off the HB.
The conclusion that on average metal poor (OoII group) are older than the richer clusters has been made
 in different studies (e.g.: Lee \& Carney 1999b).

\section{Conclusions}

Physical parameters of astrophysical relevance have been derived for the RR Lyrae stars in M2
using the Fourier decomposition of their light curves.
The estimates of the stellar radii for RRab stars
from the above approach are about 5\% smaller than radii derived from Period-Radius-Metallicity
relations obtained from nonlinear convective models, i.e.
a completely different set of pulsational models and approach. The agreement for the RRc is
generally good but the dispersion is markedly larger.

Previously recognized trends between the cluster mean values of $log~(M/M_{\odot})$, $log~(L/L_{\odot})$,
 $log T_{\rm eff}$ and $M_V$ against [Fe/H], obtained from RRc stars, have been established
for a sample of 7 OoII and 5 OoI clusters. We extended the study of the
 trends for RRab stars in 4 OoII and 5 OoI clusters.

Our analysis, based on a larger data set than previous studies, allows one
to quantify the relations (see eqs. 14-19 and Figs.
 10 and 11). In particular, much has been discussed about the relation between
 luminosity (or  $M_V$) and metallicity for the RR Lyrae variables. Our eqs. 15, 17, and 19 are in very good
  agreement with the slopes of $M_V - [Fe/H]$ relations solidly determined
and available in the literature. The zero points indicate however
that the luminosities for the RRc and RRab stars, as calculated from eq. 3 (Simon \& Clement 1993) and
 those derived from eqs. 7 and 9 (Kov\'acs 1998; Kov\'acs \& Jurcsic 1996) respectively,
 differ by the equivalent to 0.2 mag. This suggests these calibrations need to be revised.

RR Lyrae Fourier light curve decomposition produces a zero point of the
RR Lyrae distance scale consistent with those from other methods. When
the light curve decomposition technique is used on families of OoI and OoII globular
clusters, it provides physical parameters, as a function of the metal content of the cluster, that
are consistent with general notions of stellar evolution in the HB and of early stages of galactic formation.

\section*{Acknowledgments}

The authors wish to thank S. Morgan for a careful reading of a first draft of the manuscript.
We thanks the referee to have pointed Bono et al. (1995) paper to our attention.
 AAF acknowledges support from DGAPA-UNAM grant through project IN110102 and is
  thankful to the Universidad de La Laguna and the Instituto de Astrof\1sica de
  Canarias (Spain) for hospitality. EP acknowledges support from Progetto INAF 39/2005.
   We thank Juan Carlos Yustis for assistance in manouvreing Figs. 5 and 6. This
    work has made a large use of the SIMBAD and ADS services, for which we are thankful.

redpajama_set_name: RedPajamaArXiv


Updated: Feb. 11, 2019, 12 p.m.
I found out something interesting this week John Grisham and his wife have Alpha-Gal from the deer tick just like I do. They have a home in West Virginia and that is where the ticks love to be.


text:
using System;

namespace SyncTool.FileSystem
{
    public static class FileReferenceExtensions
    {
        public static bool Matches(this IFileReference reference, IFile file)
        {
            if (reference == null)
                throw new ArgumentNullException(nameof(reference));

            if (file == null)
                throw new ArgumentNullException(nameof(file));

            return StringComparer.InvariantCultureIgnoreCase.Equals(reference.Path, file.Path) &&
                   (!reference.LastWriteTime.HasValue || reference.LastWriteTime == file.LastWriteTime) &&
                   (!reference.Length.HasValue || reference.Length == file.Length);
        }
    }
}


Ethereum is currently undergoing a chain-split after a planned upgrade was called off at the very last minute.
Meaning that more than 10% of miners are on Constantinople, that being twice the amount of current miners on ETC.
An estimated quarter of a million has been lost by these miners as they are about 1,000 blocks behind. Cons-chain difficulty, however, is going down.
With it now being some hours that the cons-chain is running, it is unclear whether this is just an accidental split on the part of some miners or whether they're intentionally keeping the chain going.
Why they would be doing the latter is not very clear as one can't easily see a market for Cons, but it may be that some miners think they'd get more eth per block in the minority chain rather than in the majority chain as the difficulty bomb has kicked in.
It is far more likely, however, that they just don't know there has been a change. Some miners are in China, some in Argentina, some are across the globe.
Information tends to spread within about a week between major languages. For smaller countries/languages, two or three weeks is more probable.
It may thus be just smaller non-english speaking miners in non-major languages, like say Italy, who just don't yet know there has been any change.
Whether this is now an emergency situation isn't very clear, but we would urge great caution if you are transacting at this time because it isn't very clear whether transactions can be replayed.
This situation should now resolve within a few hours, so unless you must transact, we'd suggest just waiting for 36 hours or so to see how the picture settles.


Use a quart-sized container--like a Tupperware liquid container with lid and pouring spout. Mix all ingredients well, and personalize the amounts. Add your blood type's healing spices instead of the garlic, onion, or curry. Keep in refrigerator. It is safe, if refrigerated, for 3-4 weeks. If it's too thick, reduce the Olive Oil and increase your other oil, or add more water.
Lemon-based salad dressing that's BETTER than Oil & Vinegar and a VERY healing way to get your good oils into your diet. Do not use Flax oil.