text:
enquiries@swindonbsr.co.uk
What Is BSR?
Benefits Of BSR
The Body Stress Release Association (UK) and it's practitioners are members of the British Complementary Medicine Association (BCMA).
Swindon BSR is led by Steve Nyahwa.
BA Hons
Cert Ed
MBCMA
The specially designed BSR couch helps support your spine and prevents the need to roll over during treatment.
I first studied physiology, psychology at Chester University and in America an SUNY Plattsburg. My studies focussed not only on elite sports performance but on rehabilitation and injury prevention.
My career in fitness management and wellbeing has spanned over 20 years, firstly as a manager of spa's and healthclubs before becoming a trainer and educator within the health and fitness industry and a qualified teacher in 2010.
I have always enjoyed working with people, helping them make changes to their lives. I am grateful that I can use my knowledge and skills to improve people's quality of health, mobility and mental wellbeing.
The positive benefits of BSR became evident when my daughter was suffering from debilitating daily migraines and headaches. Over a period of four years we tried a number of remedies available through the NHS, a catalogue of medicines and a number of different complementary techniques until we came across BSR.
The regular BSR sessions helped my daughter reclaim her life, regain her confidence and independence. The headaches still occur periodically, but she is independent of medication and the headaches are less severe and far less frequent.
The success of the BSR with my daughter inspired me to leave my job and train to become a practitioner in this unique complementary technique. Becoming a BSR practitioner was the natural step for me to take.
Steve's career journey has now come full circle and he is now focussing on health and rehabilitation once again, working as a Body Stress Release practitioner, where he is able to give people unique personal advice and guidance, based on his wide-ranging experience and his driving desire to help people improve their wellbeing both mentally and physically.
To find out a bit more about BSR have a listen to this interview on BBC Radio 5 Live between Nicky Campbell and Steve Nyahwa.
Our practice is open from:
Monday-Friday 8am to 6pm
(Appointments are available outside of these hours by request)
1st appointment: allow 60 mins
Your first visit will include a detailed consultation where details of your condition, lifestyle and medical history will be taken. No special preparation is required. You are fully clothed throughout the BSR session.
Further appointments: allow 45 mins
BSR is a process helping you to retore your wellbeing. For BSR to be most effective you will require a minimum of three visits, taking place over the first two weeks. Subsequent visits will be discussed and planned according to your individual needs.
Physical injury, aches, pains and emotional stress are often a part of our everyday lives. BSR can help relieve this pain, restore your mobility and improve your emotional wellbeing.
If you would like to learn more or book a free consultation
Steve Nyahwa
Swindon Body Stress Release
Email: enquiries@swindonbsr.co.uk
Home | What Is BSR? | About Us | Benefits Of BSR | Our Clients
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docked tails and small, oval feet.
Coat: The Standard Poodle has a distinctive fine, frizzy, woolly coat similar in texture to sheep's wool.
Solid white is most common, but the coat may also be solid grey, brown, apricot, or black.
visitors, but are generally friendly toward them.
they emigrated to Australia, then subsequently to the United States during the 1849 California gold rush.
can be straight or slightly wavy, and is highly weather resistant.
Australian Shepherds are affectionate and kindhearted.
popularity, particularly with those who suffer from pet related allergies.
Size: The Aussiedoodle can vary in sizes depending upon the size of the poodle breed used in the mix.
However, they generally range from 10-25 inches shoulder height and can weigh between 15-65 pounds.
clipping. AussieDoodles with a loose wave require monthly brushing more often for curly coats.


Globally, the Foreign Account Tax Compliance Act and Common Reporting Standard regulations are profoundly affecting financial institutions. Moreover, wide varieties of entities are included in the broad definition of financial institution. Financial institutions will be required to comply with these reporting rules under the proposed legislation and will need to have procedures in place to identify accounts held by tax residents of various foreign jurisdictions and to report information annually to the Canada Revenue Agency beginning in May 2018.
If you work in the financial industry, you need to be kept apprised of ongoing regulatory developments and the latest updates to ensure that you are reporting ready for this coming year. Attend Canada's most comprehensive CRS compliance program designed for busy financial services professionals like you.
Network among your colleagues, peers and prospective clients.
Don't miss this opportunity for professional development. Register your team today!


text:
Thomas Devine Smith III (* 30. Oktober 1931 in Sabinal, Texas; † 17. Mai 2022 in Oklahoma City, Oklahoma) war ein US-amerikanischer Sportschütze und Oberstleutnant der United States Air Force.

Karriere
Thomas Smith kam in Sabinal als Sohn von Thomas Devine Smith II und dessen Frau Mary auf die Welt. Er wuchs in San Antonio auf und kam als Teenager mit dem Schützen Adolf Topperwein in Kontakt und erlernte von ihm das Pistolenschießen. Smith besuchte die Alamo Heights High School und studierte danach an der Abilene Christian University.

1953 trat Smith der United States Air Force bei. In seinen 17 Jahren bei der Luftwaffe wurde er 16 mal befördert. Am 13. Januar 1966 war Smith Pilot eines Militärflugzeugs, welches vom türkischen Izmir nach Neapel in Italien flog. Als das Flugzeug mitten im Flug explodierte, stürzte Smith ohne Fallschirm aus 1.525 Metern in die Tiefe und landete auf dem schneebedeckten Aroania in Griechenland. Als er nach mehreren Stunden der Bewusstlosigkeit wieder aufwachte, brachte er mehrere Überlebende zum Heck des Flugzeugs, das in der Nähe lag und deckte sie mit Fallschirmen zu. Von den fünf anderen Überlebenden starben zwei in der ersten Nacht. Smith war unterkühlt, also fing er an zu trainieren, um sich warmzuhalten, und blieb über 48 Stunden wach. Er legte einen roten Fallschirm als Markierung aus, wodurch die Gruppe schließlich nach drei Tagen und zwei Nächten gerettet werden konnte. Smith und drei weitere Personen überlebten. Für diese Leistung wurde Smith vom General Bruce K. Holloway, dem Oberbefehlshaber der United States Air Forces in Europa, die Airman's Medal verliehen. 1979 beendete Smith seine militärische Laufbahn als Oberstleutnant.

Als Sportschütze war Smith bei den Panamerikanischen Spielen 1963 sehr erfolgreich. Dort gewann er Gold mit der Großkaliberpistole sowohl im Einzel als auch mit der Mannschaft. Mit 597 von möglichen 600 Punkten übertraf er dabei zudem den bisher bestehenden Weltrekord von 591 Punkten. Bei den Olympischen Spielen 1968 wurde er im Wettkampf mit der Freien Pistole Achter.

Nach seiner Militärkarriere zog Smith nach Buffalo, Wyoming, und heiratete dort seine Frau Ann Cusak. Nach dem Tod seiner Frau zog er nach Oklahoma City. Dort lernte er 1986 seine zweite Ehefrau Barbara kennen, die er drei Jahre später heiratete. Smith trat dem OKC Safari Club bei und war dort zwei Jahre als Präsident aktiv. Später war er bei der Ausbildung von militärischen Scharfschützen der Oklahoma Highway Patrol tätig.

Weblinks

 Nachruf (englisch)

Sportschütze (Vereinigte Staaten)
Olympiateilnehmer (Vereinigte Staaten)
Teilnehmer der Olympischen Sommerspiele 1968
Teilnehmer an den Panamerikanischen Spielen (Vereinigte Staaten)
Panamerikaspielesieger (Sportschießen)
Oberstleutnant (United States Air Force)
US-Amerikaner
Geboren 1931
Gestorben 2022
Mann

redpajama_set_name: RedPajamaWikipedia


This link will take you to our Square Payment system.
You can donate for this ministry event online through the Joy Square payment system. We have set-up various financial donation options. This will assist us in buying materials to make the bunk beds.
The approximate cost in materials to build a single bunk bed is $200. Your donations help defray the cost of materials for future bunk bed builds and helps keep this ministry vibrant.
You can also donate for the ministry event at the door (please register online)!


Reports on the decision of the Personal Communications Industry Association to change its name to PCIA. Tag line added to the name of the organization; Reason for changing the name of the organization; Objective of the organization.
Reports on the availability of the Global M-User Market Research from the Personal Communications Industry Association in September 2001. What the market research data provides companies.
Reports on the reorganization of the Personal Communications Industry Association into PCIA. Tagline of the association; Board members of the organization; Response of small tower companies on the formation of the group; Actions taken by the association regarding concerns of small companies.
Announces the conference of the Personal Communications Industry Association on October 23, 2002. Scheduled topics of discussion.
Focuses on the outcome of the 2000 GlobalXChange convention of the Personal Communications Industry Association (PCIA). Comments from convention participants; What trade shows do; Recommendations for future shows of the PCIA.
Focuses on the 1995 Personal Communications Industry Association-sponsored show or PCS '95. Highlights of the show; Telecommunication companies participating in the show; Objectives of the show.
Comments on the PCS 1999 convention held by the Personal Communications Industry Association (PCIA). Mergers of wireless companies; Views of AOL Interactive Properties Group president, Ted Leonsis on the convergence of wireless communication and the Internet; Highlights of the convention.
Reports on the move of Personal Communications Industry Association (PCIA) to focus efforts on private radio and towers. Background of PCIA; Details of PCIA membership sections.


Before switching to Applied technology, ChurchWest partnered with one of their insurers, taking on their book of business. This partnership required a management system that had the ability to operate two agencies seamlessly. ChurchWest's previous system did not allow this scalability, so they decided to look into other agency management systems.
I am a strong believer that you want all of your data and processes in one system. Whether it's sales, benefits, accounting, receptionist processing calls, if everything is in one system, it's infinitely more efficient. And because the system is so efficient, it frees us up to do more marketing.
ChurchWest chose Applied Epic to manage their business. Applied Epic is the most technologically advanced cloud-based software application built for independent insurance agencies to automate business operations and drive connectivity to insurers and insureds in the changing insurance marketplace.
A single management system with essential capabilities for the entire agency.
ChurchWest leverages sales automation through Applied Epic to view, monitor, track and forecast new business opportunities and renewals directly within the application. "Everyone knows the importance of having an active pipeline," continued Lucas. "We have about 11 different campaigns running at all times. Our producers are in awe that they don't have to search for prospects every day. The system itself is driving it for them. We also measure phases of sales cycle – every appointment we set up, we can see if it turns into a quote. It's really allowed us to enhance our sales pipeline." Since leveraging Applied Epic, ChurchWest has been able to double in premium in just five years and their customer retention ratio has risen from 94% to 97%.
Utilizing sales automation, staff at Weatherby-Eisenrich Insurance easily manage their pipeline.
Leveraging a single agency management system, BHS Insurance automates their entire business.


text:
Chicago Cubs Requesting "Wrigleyville" Atmosphere; Decision to Stay in Mesa or Move to Florida Expected by the End of the Week
It's coming down to the wire, and Chicago Cubs President Crane Kenney says a decision on whether the team will keep its spring-training facilities in Mesa or move it to Naples, Florida, will be made "in the very near future.
Kenney met with lawyers and Mesa city officials this morning to discuss two potential sites for the Cubs' spring training facilities in Mesa and told ESPN's Bruce Levine that a decision could be expected by the end of the week.
Naples, however, has three potential sites for the Cubs to consider, and getting a hold of the projected $80 million needed to create what the Cubs want may be easier in Florida -- where the money would come from the County Tourist Development Center -- than in Arizona.
For the Cubs to get what they want, it would take state and county referendums here to come up with the money needed.
Getting the necessary legislation to secure the money would only take 45-90 days in Florida, according to Levine, while in Arizona, securing the same amount of money could take up to six months.
What the Cubbies want is a mini-Wrigley Field in the middle of whatever city they decide on.
The Cubs are expecting 50,000 square feet for a facility that will include a 15,000-18,000-seat stadium, which would be the largest capacity of any spring-training facility. They also want to create a "Wrigleyville," atmosphere, complete with new restaurants, hotels, bars and retail outlets that would create an ambiance similar to that around the iconic Wrigley Field in Chicago.
Check back tomorrow for any new developments.

redpajama_set_name: RedPajamaCommonCrawl


text:
package org.fit.vutbr.relaxdms.api.service;

import com.fasterxml.jackson.databind.JsonNode;
import java.util.List;
import java.util.Set;
import org.fit.vutbr.relaxdms.data.db.dao.model.Document;
import org.fit.vutbr.relaxdms.data.db.dao.model.workflow.Environment;
import org.fit.vutbr.relaxdms.data.db.dao.model.workflow.LabelEnum;
import org.fit.vutbr.relaxdms.data.db.dao.model.workflow.StateEnum;
import org.fit.vutbr.relaxdms.data.db.dao.model.workflow.Workflow;

/**
 *
 * @author Martin Kanis
 */
public interface WorkflowService {

    /**
     * Returns workflow from document specified by id.
     * @param docId Id of document which workflow will be returned
     * @return Workflow Workflow of document
     */
    public Workflow getWorkflowFromDoc(String docId);

    /**
     * Returns workflow from json document
     * @param doc Document as JsonNode
     * @return Workflow of the document
     */
    public Workflow getWorkflowFromJson(JsonNode doc);

    /**
     * Approves document by setting property in workflow
     * @param docData Metadata and workflow of the document
     * @param user User who approves document
     */
    public void approveDoc(Document docData, String user);

    /**
     * Declines document by setting property in workflow
     * @param docData Metadata and workflow of the document
     * @param user User who declines document
     */
    public void declineDoc(Document docData, String user);

    /**
     * Checks if document is approved
     * @param workflow
     * @return boolean
     */
    public boolean isApproved(Workflow workflow);

    /**
     * Checks if document is declined
     * @param workflow
     * @return boolean
     */
    public boolean isDeclined(Workflow workflow);

    /**
     * Checks if state of document matches expected state.
     * @param workflow Workflow
     * @param expectedState StateEnum
     * @return boolean True if expected state is the same as actual state of document
     */
    public boolean checkState(Workflow workflow, StateEnum expectedState);

    /**
     * Checks if document's labels contain expected label.
     * @param workflow Workflow
     * @param expectedLabel LabelEnum
     * @return boolean True if expected label is one of the document's labels
     */
    public boolean checkLabel(Workflow workflow, LabelEnum expectedLabel);

    /**
     * Changes state of provided document to expected state
     * @param docData Document metadata
     * @param expectedState StateEnum
     * @param user Use who changes state
     */
    public void changeState(Document docData, StateEnum expectedState, String user);

    /**
     * Assigns document to given user.
     * @param docData Document metadata
     * @param assignee Assignee of document
     */
    public void assignDocument(Document docData, String assignee);

    /**
     * Adds workflow to the json document.
     * @param doc Document where to put workflow
     * @param workflow Workflow to be added to the document
     * @return Document with added workflow
     */
    public JsonNode addWorkflowToDoc(JsonNode doc, Workflow workflow);

    /**
     * Adds label of specified type to the document.
     * @param docData Document metadata
     * @param labelType Type of label
     * @param user User who adds label to the document
     */
    public void addLabel(Document docData, LabelEnum labelType, String user);

    /**
     * Checks if the document can be signed.
     * @param docData Document metadata
     * @param isManager Boolean Is logged user manager
     * @return boolean
     */
    public boolean canBeSigned(Document docData, boolean isManager);

    /**
     * Inserts metadata and workflow from all documents to the drools engine as facts.
     * @param docDataList List of Documents
     * @param env Additional data for drools engine
     */
    public void insertAllFacts(List<Document> docDataList, Environment env);

    /**
     * Serialize provided json to workflow object.
     * @param json String
     * @return Workflow
     */
    public Workflow serialize(String json);

    /**
     * Submits document to manager via Drools.
     * @param docData Document
     * @param env Additional data for drools engine
     */
    public void submitDocument(Document docData, Environment env);

    /**
     * Checks if document is submitted
     * @param workflow
     * @return boolean
     */
    public boolean isSubmitted(Workflow workflow);

    /**
     * Checks if user is authorized to see/write document.
     * @param docId Id of document
     * @param user User
     * @return boolean
     */
    public boolean isUserAuthorized(String docId, String user);

    /**
     * Add provided user to the document permissions.
     * @param docData Document
     * @param elligibleUser User to be elligible to the document
     */
    public void addPermissionsToDoc(Document docData, String elligibleUser);

    /**
     * Returns all permissions from document.
     * @param docData Document
     * @return Set of usernames
     */
    public Set<String> getPermissionsFromDoc(Document docData);

    /**
     * Returns list of rules in the customWorflow.drl file.
     * @return List of rule's names
     */
    public List<String> getCustomRules();

    /**
     * Checks if document specified by Id is protected from editing.
     * @param docId Id of document
     * @return True if document can't be edited.
     */
    public boolean isReadOnly(String docId);
}

redpajama_set_name: RedPajamaGithub


text:
A superb 4 court sports hall available to hire in Little Heath Romford. Perfect for Football, Badminton, Netball, Handball and much more.
The Sports hall measures approx., 33m x 18m and has a dividing curtain as well as markings for Football, Basketball, Badminton , volleyball and netball.
Prices from £35 per hour. (Please note that bookings maybe subject to VAT and pricing for events and large bookings may differ)
For more information contact our bookings team today or submit an online enquiry form
Enquire for Sports Hall
Thank you, we've received your message and will respond as soon as possible.
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A superb 4 court sports hall available to hire in Little Heath Romford. Perfect for Football, Badminton, Netball, Handball and much more,
Full Details & Booking
Activity Studio
A versatile Activity Studio available to hire in Romford, RM6 4XX
Assembly hall
A fantastic Assembly hall perfect for meetings, conferences, celebrations and events. Located in Romford it is a perfect space for the community to use.
An adaptable teaching space to hire in Romford, perfect for tuition groups, private lessons, meetings and much more
22 Sep 08:00 - Today marks the 10th Anniversary of National Fitness Day. National Fitness Day encourages the nation to celebrate t… https://t.co/e0ZnR2j3QO
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© 2022 5002 - ATAM Academy
Registered Company: ATAM Academy, Little Heath, Romford, RM64XT


Ember, the new guilt-free biltong brand is adding a new 'shot' format to the range from next month. The 16g mini packs contain 10g protein and offer bite-sized slices of biltong in an on-the-go format, a first for the Biltong and Jerky category. All Ember products are sugar-free, gluten-free, low in calories and available in two flavours; Original and Chilli.
In a major win for the brand, it has also secured three national supermarket listings with Ocado, Sainsbury's and Waitrose for the full range after just six months in the market. The shots will launch in 212 Sainsbury's stores from 8th April followed by 297 Waitrose stores from 25th with the bigger 30g bags launching in the snacking aisle in 270 Waitrose (30th April) and Sainsbury's (July). Ocado will be listing the full range from 30th April.
Ember has seen phenomenal success since it launched in October 2017, with sustained revenue growth of 65% month on month. Not only has it become the No.1 meat snack brand on Amazon, but by July will have more than 3,000 distribution points in the UK, (including key accounts such as Brewdog and Musclefood and by the end of 2018 they are expecting to have sold 1.5 million bags of Biltong.


text:
Mladostništvo ali adolescenca je razvojno obdobje pri človeku med otroštvom in odraslostjo. Kronološke opredelitve in stroka pri določanju spodnje in zgornje meje adolescence niso enotne. Začne se z nastopom pubertete in konča z vstopom v odraslost, torej približno med 11. (za dečke 13.) in 20.- 24. letom starosti. Beseda »adolescenca« izvira iz latinskega pridevnika »adolescens«, doraščajoči

Razvojni mejniki mladostništva
Adolescenca se pri dekletih začenja z enajstim letom in traja do šestnajstega, pri fantih to obdobje traja od dvanajstega do osemnajstega leta. Razvojno obdobje adolescence delimo na dve stopnji - predpuberteto in puberteto. Kot prehod med otroštvom in adolescenco velja nastop pubertete, ki pomeni doseganje reproduktivne zrelosti in ga kažejo navzven očitni znaki: hitra telesna rast (t. i. rastni sunek) ter razvoj sekundarnih spolnih znakov. Čeravno ne nastopi pri vseh posameznikih v istem obdobju, pa gre za opazen in individualno jasen vstopni mejnik. Velja, da pri dekletih nastopi prej kot pri dečkih.

Nastop in vrhunec rastnega sunka se pri dekletih začne malo pred 11. letom starosti in doseže vrhunec pri 12 letih; za dečke pa velja, da nastopi okoli 13. leta in doseže vrhunec pri 14. letih.

Na drugem koncu smo soočeni z večjimi težavami pri opredelitvah. Težko je jasno določiti, kdaj je nek posameznik psihološko odrasel. V splošnem lahko trdimo, da je posameznik odrasel, ko je

 (1) sposoben samostojno preživeti ter hkrati
 (2) poskrbeti za reprodukcijo vrste (ustvariti družino, skrbeti za naraščaj),

torej ko izvaja obe funkciji (brez težav ali regresij). Sredi 20. stoletja in vse do 70. oziroma 90. let (odvisno od družbenega konteksta) so konec adolescence in prehod v odraslost strukturirale srednje šole (matura kot zrelostni izpit), dandanes pa so ti prehodi mnogo manj jasni.

Ali se bo večina populacije pri določeni starosti npr. zaposlila oziroma ali si bo ustvarila družino ali pa bodo te značilnosti močno razpršene ter kako se funkciji odraslih konkretizirata v neki družbi, je močno odvisno od razmerij znotraj te družbe, kulture, od navad ipd. Danes odraslost subjektivno označuje samostojnost odločanja o sebi in svojih dejanjih, ekonomska neodvisnost in samostojno življenje.

Razvojne naloge
Za uspešen socialni razvoj in subjektivno zadovoljstvo mora mladostnik v obdobju adolescence obvladati skupek znanj, spretnosti in načinov vedenja, da bi se kot posameznik razvil v zrelega odraslega. Med pomembne razvojne naloge, ki jih mora mladostnik usvojiti sodi sprejemanje hitrih telesnih sprememb, doseganje čustvene neodvisnosti, oblikovanje socialne spolne vloge, oblikovanje odnosov z vrstniki, razvoj odgovornega vedenja, poklicni cilji, partnerstvo in družina, vrednostne usmeritve.

Razvoj identitete v mladostništvu
Splošno prepričanje je, da je adolescenca razvojno obdobje, čas, ko mladostnik oblikuje svojo  identiteto. Oblikovanje identitete je psihološki proces, v katerem se posameznik opredeli glede lastnosti in značilnosti, za katere verjame, da predstavljajo njega samega. S poudarkom na razumevanju samega sebe in razumevanju lastnih usmeritev v prihodnosti. Mladostnik v tem obdobju kot pomemben del v strukturi identitete oblikuje »pojem o sebi«, ki združuje vrsto značilnosti, lastnosti, stališč, vrednot, sposobnosti za katere je prepričan, da ga opredeljujejo. Pri mlajših mladostnikih »pojem o sebi« vsebuje predvsem socialne in značajske lastnosti (sem lepa, sem pameten), pri starejših mladostnikih pa so izpostavljeni individualni cilji in načrti za prihodnost.

Vrednostni vidik pojma o sebi je »samospoštovanje«, ki v povezavi s čustvi izraža odnos do lastne vrednosti. V adolescenci se samospoštovanje kot vrednostna sodba nanaša na lastno učno uspešnost, telesne sposobnosti, socialno vrednost, na všečnost do nasprotnega spola, raznovrstna prijateljstva. Stopnja samospoštovanja med mladostniki je zelo različna. V šoli manj uspešni mladostniki imajo nižje samospoštovanje, višje pa mladostniki iz materialno dobro stoječih družin. V razvojnem obdobju adolescence mladostnik potrebuje čas, da kot opazovalec lastnih sprememb, psiholoških in na svojem telesu, vse te spremembe poveže v celoto, v identiteto jaza. Mladostniki sprejme samega sebe, lastno individualnost.

Dosežene identiteta mladostnika ni nekaj končnega, vsebuje zmožnost ponovne opredelitve. Lahko se dopolni, popravi, spremeni glede na družbeno vlogo in pojmovanje samega sebe kot posameznika v družbi. Ponovno opredeljevanje pa je v tesni povezavi z uspešnostjo obvladovanja identitetne krize v mladostništvu.

Odnosi v mladostništvu
Mladostnik v obdobju adolescence količinsko in kakovostno spremeni odnose z vrstniki, drugimi člani družine, starši in z ljudmi v okolju v katerem živi. V komunikacijo s širšim okoljem vlaga veliko energije in koncentracije. Prednostna razvojna naloga mladostnika je osamosvajanje od staršev in ustvarjanje odnosov z vrstniki. V ospredju so prijateljstva in intimnimi odnosi s partnerji. Število in intenzivnost konfliktov med mladostnikom in starši je v obdobju mladostništva večje. Razumljivo je, da mladostnik in starši ne delita istih pogledov na različne življenjske situacije. Običajno so različna mnenja in razhajanja občasna do zmerna in imajo pozitivno vlogo pri osamosvajanju mladostnika. Vzporedno pa oblikovanje odnosov z vrstniki pomembno vpliva na mladostnikovo osamosvajanje od družine in na oblikovanje lastne identitete, na njegovo vedenje, socialne spretnosti, zmanjšanje mladostniškega egocentrizma in na razvijanje  njegovih odnosov z nasprotnim spolom. Prijateljstva v tem obdobju temeljijo na zaupanju, iskrenosti, odprtosti, čustveno so zelo nabita in intenzivna. V zgodnjem obdobju mladostništva so na prvem mestu telesna privlačnost in prvi vtis, ki ga naredijo na vrstnika, v srednjem prijateljstvo, intimnost, ljubezen, spolne izkušnje, v poznem obdobju adolescence pa razumevanje, skupni interesi, intimnost in podobni načrti za prihodnost.

Osamosvajanje od staršev
Mladostnik v procesu osamosvajanja od staršev preizkuša lastne vzorce vedenja. Spremembe v odnosu mladostnik in starši se odražajo v izmenjavi konfliktov in čustvene povezanosti. Svojo različnost od staršev mladostnik med drugim dokazuje z odklanjanjem starševskih nasvetov in zavračanjem njihovih stališč. Svojo voljo izraža z lastnimi vzorci vedenja, z izbiro glasbe, ki jo posluša, z uporabo slenga, govorice mladih, s spremenjenim zunanjim, videzom, ki ga poudarja z drugačno pričesko ali modnim slogom. Mladostnik odnose z vrstniki umešča na prvo mesto. Na čustvenem področju se v obdobju osamosvajanja mladostnikova potreba po čustveni opori in psihološki bližini staršev zmanjšuje. Vzporedno pa se povečuje mladostnikovo hotenje po oblikovanju lastnih stališč, lastnega sistema vrednot, ki se razlikuje od starševskega. Pomemben del osamosvajanja mladostnika od staršev je njegovo spoznanje, da so starši osebnosti, ki imajo svoja prepričanja, dobre in slabe lastnosti, da niso idealni in da je starševstvo le ena od socialnih vlog, ki jih starši kot posamezniki opravljajo.

Odnosi z vrstniki
V obdobju mladostništva postajajo odnosi mladostnika s posamezniki podobne starosti, podobnih pogledov in prepričanj vse bolj pomembni. Za mladostnika je značilno, da si z vrstniki izmenjuje čustva, razpoloženja in doživljaje. Mladostnika z vrstniki povezujejo osebnostne značilnosti, skupni interesi in želje, z njimi razpravlja o prihodnosti in svojih ciljih. Z vrstniki si deli in pridobiva informacije o tistih področjih svojega življenja o katerih se s starši bolj malo ali redko pogovarja. Mladostnik z vrstniki veliko komunicira. Številni telefonski pogovori brez konca in kraja so ena najpomembnejših mladostnikovih socialnih dejavnosti. Pogovori na daljavo, množica elektronskih sporočil so pokazatelj priljubljenosti posameznika in hkrati dokaz kako visoko je mladostnik uvrščen v skupini vrstnikov. Mladostnik z vrstniki preživi veliko prostega časa, skupaj sodelujejo v različnih športnih in drugih aktivnostih. Skupno druženje in preživljanje prostega časa močno vpliva na mladostnikov socialni razvoj.

Vrstniki lahko tudi negativno vplivajo na mladostnika, če ga zavračajo, odrivajo iz družbe ali mu namenjajo žaljive opazke in se iz njega norčujejo.

Prijateljstva
Pomemben del mladostnikovega življenja so prijatelji in prijateljstva. Prijateljske zveze so običajno čustveno tesne in psihološko močne. Prijateljstva v razvojnem obdobju mladostništva so omejena na istospolna prijateljstva, na dekliška in fantovska. Prijateljske povezave temeljijo na podobnih osebnostnih lastnostih, značilnostih, podobnih interesih in pogledih na prihodnost. Mladostnikovi pogovori s prijatelji so odkriti, zaupni, iskreni. Prijatelji se pogovarjajo o doživljanju in razumevanju lastnih čustev, dojemanju in spoznavanju intimnih plati življenja, razmišljajo o prihodnosti, o konfliktnih situacijah, delijo si nasvete in izmenjujejo informacije o tem kakšen vtis o mladostniku imajo prijatelji.

Dekliška prijateljstva v razvojnem obdobju mladostništva so tesna, notranje povezana in intimna. Prijateljstva med fanti, povezujejo jih skupno zanimanje in skupne dejavnosti, so v primerjavi z dekliškimi bolj številčna.

Egocentrizem v mladostništvu

Mladostniški egocentrizem običajno povezujemo s predstavo namišljenega občinstva in osebne zgodbe. Mladostnik namreč zelo pogosto intenzivno razmišlja o tem kako ga vidijo drugi in kakšen vtis naredi na svoje vrstnike. Obratno tudi njegovi  vrstniki razmišljajo predvsem o tem kakšen vtis naredijo na druge. Mladostniki so v bistvu opazovalci, predvsem in najprej opazujejo sebe in precej manj druge. Mladostnik sebe postavlja v središče dogajanja, na oder. Pri tem se ne zaveda, da njegovi vrstniki in drugi posamezniki o njem ne razmišljajo toliko in na tak način kot on sam. Po drugi strani mladostnik o sebi ustvarja svojo osebno zgodbo. Idealizira svoje lastnosti in zgrešeno verjame, da je kot posameznik nekaj posebnega, izstopajočega in da ima edinstvene sposobnosti, ki mu omogočajo, da se znajde v vsaki situaciji. Nekateri mladostniki se tako izpostavljajo različnim pozitivnim in negativnim vplivom okolja in do skrajnosti preskušajo svoje telesne zmožnosti.

Nerealne predstave o sebi vplivajo na mladostnikovo prepričanje, da ga nihče ne razume in da zanj v družbi veljajo drugačna socialna pravila.

Adolescenca skozi zgodovino

Večina tradicionalnih družb mladostnikom kot osebam v težavnem obdobju ne namenja veliko pozornosti. Prehod iz otroške dobe v odraslost je pogosto pospremljen z rituali, ki simbolno označujejo prehod iz enega starostnega obdobja v drugo. Prehod z rituali je reintegracija - ponovno doseganje ravnovesja osebnosti - mladostnika v družbo, vendar z novim spremenjenim statusom.

Proti koncu 18. stoletja je tudi v "zahodnih" družbah veljalo, da otrok prestopi v odraslo dobo s prevzemom obveznosti in dolžnosti, ki mu jih narekuje družbeni razred kateremu pripada. V tem času umetnostne, literarne in slikarske, upodobitve prikazujejo otroke kot "majhne odrasle" oblečene v enaka oblačila kot odrasli.

Ob izteku 19. stoletja so v nekaterih evropskih državah, predvsem v Nemčiji, Angliji, Franciji, globoke ekonomske in socialne spremembe vplivale na položaj in življenjske pogoje odraščajočih. Spremeni se pogled na pomen izobraževanja, ki postaja vse bolj pomembno. Povečuje se število šol in različnih izobraževalnih ustanov, podaljšuje se obdobje učnih praks in izobraževanja. Vzporedno doživljamo razcvet literature o adolescenci in za adolescente, nastajajo nove institucije, združbe in organizacije namenjene samo mladim in za mlade, taborniki, skavti ... .

Kot odgovor na nujnost ustvarjanja identitete v novem življenjskem razvojnem obdobju adolescenca dobi drugačen družbeni pomen. Del strokovne javnosti se s takšno opredelitvijo adolescence ne strinja, češ da je faza adolescence izum moderne družbe, ki  negativno vpliva na mlade, v smislu podaljševanja obdobja dozorevanja.

Opombe

Glej tudi
 razvojna psihologija

Viri

 Arnett, Jeffrey Jensen, Emerging Adulthood: A Theory of Development From the Late Teens Through the Twenties. American Psychologist, 2000, 55, št. 5, str. 469-480.
 Arnett, Jeffrey Jensen, Suffering, Selfish, Slackers? Myths and Reality About Emerging Adults. Journal of Youth and Adolescence, 2007, 36, št. 1, str. 23-29.
 Coleman, J. C. in Hendry, L., The Nature of Adolescence. Second editon. New York, London, Routledge, 1990.
 Erikson, Erik Homburger, Identity: Youth and Crisis. New York, London: W. W. Norton & Company, 1994.
 Fasick, Frank A., On the »Invention« of Adolescence. Journal of Early Adolescence, 1994, 14, št. 1, str. 6-23.
 Galland, Olivier, Les jeunes. Paris: Éditions La Découverte, 1993.
 Gillis, J. R., Mladina in zgodovina. Šentilj: Aristej, 1999.
 Kaplan, Paul S., Adolescence. Boston, New York: Houghton Mifflin, 2004.
 Mrgole, Albert, Kam z mularijo? Ljubljana: MŠŠ, URSM in Maribor: Aristej, 2003.
 Steinberg, Laurence, Adolescence. Third edition.  New York [etc.]: McGraw-Hill, 1993.
Ule, Mirjana Nastran, Mladi v družbi novih tveganj in negotovosti. V: Šelih, A. (ur.), Prestopniško in odklonsko vedenje mladih. Ljubljana: Bonex, 2000, str. 11-32.
 Ule, Mirjana in Kuhar, Metka, Sodobna mladina: Izziv sprememb. V: Miheljak, V. (ur.), Mladina 2000 : slovenska mladina na prehodu v tretje tisočletje. Ljubljana: URSM in Maribor: Aristej, 2002, str. 39-77.
 Zupančič, Maja in Svetina, Matija, Mladostništvo. V: Marjanovič Umek, L. in Zupančič, M. (urednici), Razvojna psihologija. Ljubljana: Znanstvenoraziskovalni inštitut Filozofske fakultete, 2004, str. 510-632.

Razvojna psihologija
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text:
Q: Can't connect to MySQL with a new MySQL user I work on a personal website. I just put it on the production server. When I am in the development environment I connect to MySQL with root but now I just created a user specific for this website. So I wrote this command line in MySQL:
GRANT USAGE ON portefolio.* TO 'userPortefolio'@'localhost' IDENTIFIED BY PASSWORD 'myPasswordCrypted'

The query is ok, but on my website, when I try to access a page with a query, Symfony gives me that error:
SQLSTATE[42000] [1044] Access denied for user 'userPortefolio'@'localhost' to database 'portefolio'

I tried to restart the server to be sure everything is ok but nothing.
I encrypted the password with the MySQL function
password('my password not encrypt')

and in Symfony I wrote the password in non-encrypted format. Is that ok?

A: GRANT USAGE ON portefolio.* TO 'userPortefolio'@'localhost' IDENTIFIED BY PASSWORD 'myPasswordCrypted'

Your password should not be encrypted in this statement. MySQL crypts it automatically.

A: Assuming no quirks in connecting etc were made you should do a
flush privileges;

after running the grant query.

A: quoting from the manual: The USAGE privilege specifier stands for "no privileges."
so everything seems to be working as designed.

redpajama_set_name: RedPajamaStackExchange


Refined and luxurious, fur is the oldest material in the history of clothing. Although, in ancient times, almost every woman could wear a fur coat, as it wasn't something luxurious, but a garment of primary necessity for cold winter months, now, much has changed in the world of fashion. Nowadays, fur isn't just a symbol of luxury and wealth, a high social status and glamour, but it's also subject to all fashion trends, and trends are what make our life so exciting and beautiful. Almost no cold season could go without the fur trend. From season to season we see various fur types, new colors, new garments featuring this uber-luxurious material and new styling solutions. However fresh and gorgeous these new trends come to be, there is one thing that is unchangeable, which is the base, the material: the fur.
With fur being such a widely-spread material, which is used for creating coats, vests, hats, handbags and other clothing pieces and accessories, we begin to wonder: how to wear fur and look stylish and refined, and not trashy and bulky? Here, we present some easy style tips on wearing fur, as well as basic knowledge about how to store fur and extend the life of your favorite fur pieces.
Despite its nobility, high class and luxury, many people consider fur the ugliest material, since hundreds of animals suffer for creating genuine fur pieces. This is the reason why there is a tendency to use faux fur for creating a coat or any other garment. Besides, faux fur is much more affordable and almost any fashioniser can buy a faux fur item. Keep in mind that everything depends on styling, so if you have a faux fur item and style it right, you are sure to look like a hundred bucks.
There are various types of fur, different colors and shapes, and, of course, genuine and faux fur. In order to brighten up the exuberant, lush material, many fashion designers brought the psychedelic fur trend too, dying mainly faux fur in all the possible shades of the rainbow, from pastel tones to bright fuchsias, oranges or reds.
When choosing a fur, pay attention not only to the quality and its rich look, but also color. It's advised to go for contrasts. For example, if black and gray prevail in your wardrobe, pick something colored, such as lush green, purple or mustard, in order to add a pop of color to your look. On the other hand, if you are a fan of bright dresses and printed clothing, pick a fur accessory staying in the color spectrum: purple goes well with orange, blue " with yellow, red " with dark green. Also, if buying a fur item is something luxurious for you, choose something classy, which will hardly go out of style. All those bright and pastel colored fur items are likely to become old fashioned one day, which you can never say about brown, gray or camel tones.
• If you are so much in love with fur, you'll certainly have a fur coat. Long fur coats are more luxurious and they don't look so good with casual outfits worn every day. Instead keep this garment for special occasions. Wear it with a long elegant dress and high heels, accessorized with chic jewelry pieces and a clutch, when you plan to go to an evening party or a formal occasion.
• On the other hand, midi and short fur coats can look more practical. You can easily pair your favorite short fur coat with a pair of jeans and leather boots. Besides depending on the design of your short fur coat, it can also look quite elegant with classic clothing pieces and cocktail dresses, sported for special occasions.
• Fur tends to make one look bigger and fatter than she really is, since it's a bulky piece of clothing. To balance things, always wear something light and thin underneath fur. You'll hardly feel cold, as fur is already warm enough.
• Keep in mind that fur looks extremely luxurious and instantly catches the eye. Wearing fur from head to toe, you are likely to resemble a mink or a lynx. Keep things simple and always wear one single fur item at a time. Treat fur as a piece of accessory, an embellishment to always have a successful look.
• Psychedelic fur looks great with skinny jeans tucked into boots, as well as with leather trousers and high boots.
• Certainly the easiest way of sporting fur is going for fur accessories. Like fur coats, subtle accents of fur also look quite effective, giving a touch of nobility and chic to your look. Think fur handbags, boots with fur inserts, fur hats, fur scarves, collars, ear muffs, fur jackets or vets.
• Fur jackets are also an interesting way of nailing down the fur trend. They look especially amazing with skinny pants and high boots.
• A fur scarf, a fur hat or fur ear muffins are perhaps the most versatile fur pieces. They fit almost everyone and look good with almost any kind of clothing. Besides they are small fur accessories, and when fur is less, it's definitely more beautiful.
• Fur collars are the most fun fur accessories. Adding a fur collar on your ordinary coat, jacket or sweater, you instantly transfer your look, adding a classy touch to your outfit. You can also wear a fur scarf as a collar.
• Fur trimmed boots certainly look voguish, yet while dealing with them, always pay attention to your weight and silhouette. If you are short and plump, these shoes will definitely make you look shorter and fatter. Always opt for fur trimmed boots that contain no more than 30% of fur.
• Fur handbags, coming in various shades and shapes, can instantly add a chic vibe to your outfits. However, never try to wear a fur handbag in summer, as it's a winter accessory.
• Fur looks chic with other refined materials too, especially leather. There are even ready-made pieces that are a blend of both the materials. Fur outerwear always looks amazing with leather footwear, leather skirts and leather pants.
• To embrace the '70s style, you can wear fur with wide-leg pants and midi skirts. It can be a fur coat or a fur-trimmed coat, a fur scarf or a fur vest.
• When matching a short fur coat with a miniskirt or short shorts, you create the alluring '60s vibe, which is so cool and stylish.
• Always store your fur in summer in a special garment protector, treated with mothballs. You can also put dried orange peel or tobacco leaf into the garment protector.
• Try to store your fur in a cool dark place, so that it doesn't fall under the direct sunlight in any case.
• Opt for a massive coat hanger with a wide solid neck so that your coat doesn't sag in any case.
• Never wash you fur with washing powder, don't wash it with shampoo in the shower and don't dry it with a hair dryer.
• Don't try to remove the grease and stains with gasoline or acetone: they are the biggest enemies of fur.
• If possible, take your fur to a fur specialist once a year so that she can repair the imperfections.
• Never store genuine fur with dyed one.
• Don't hang fur on whitewashed walls, as chalk tends to spoil fur.
• Never iron your fur coat, as the slightest temperature effect changes the structure of your fur garment.
• Don't use any chemical products on your fur, such as perfume or sprays. The alcohol contained instantly gets absorbed in the fur, making it smell awful for a long time.
• If your fur garment got accidently wet in the rain or snow, don't try to dry it with any equipment quickly. Keep in mind that fur can be dried only at room temperature. Once it's completely dry, comb it with a brush.
Dear fashionisers, keep in mind that fur loves snow, frost, wind and when it's politely taken care of. Don't use perfume on your fur garments, don't wear a shoulder bag over your fur coat and don't get caught up in the rain. Don't try to wear lots of fur garments at a time or layer it a lot. Learn these easy fur styling tips and you are sure to always look enviable, chic and refined!


text:
\section{Introduction}

According to the standard inflationary cosmology, the early universe underwent a very short period of rapid accelerated expansion, which was originally assumed as a mechanism to solve several puzzles of the Big Bang theory, e.g., the flatness and horizon problems \cite{guth,sato,starob,linde1,stein,linde2}.
Inflation also provides plausible scenarios for the origin of the large scale structure of the universe, as well as the formation of anisotropies in the cosmic microwave background radiation.
We refer, e.g., to Refs. \cite{linde3,liddle,lyth} for a detailed review on the different kinds of inflationary models developed so far, including recent attempts to construct consistent models of inflation based on superstring or supergravity models.
In order to achieve inflation, the strong energy condition has to be broken (in general), so that the evolution of the universe at very early times is expected to be driven by a source field with positive energy density and negative pressure.
The simplest way to model a system with such a property is to assume a scalar field.
A variety of scalar field models of inflation have been proposed so far, including quintessence \cite{quint}, k-essence \cite{kess1,kess2}, phantom \cite{phan} and tachyonic scalar fields \cite{tach}.

The evolution of a scalar field in a given gravitational background can be equivalently described by using a hydrodynamic representation (see, e.g., Ref. \cite{lyth}).
In fact, the scalar field mainly acts as a perfect fluid, even if it cannot in general be described by an equation of state relating energy density and pressure in a standard way.
Fluids with negative pressure are indeed widely used in cosmology and string theory to describe \lq\lq exotic" matter and topological defects (associated with phase transitions in a primordial universe).
In many practical cases, they can be represented by perfect fluids with a barotropic equation of state $p=w\rho$, with negative $w$, like fluids of cosmic strings and domain walls \cite{cosm1,cosm2}.
The equivalence between field representation and hydrodynamic representation then holds at a very formal level only, and requires some care to be predictive, especially when fluids with negative pressure are involved, as discussed in Ref. \cite{fabris}.

The usual way to formulate a scalar field model of inflation is to specify a Lagrangian with prescribed kinetic and potential terms, also taking into account the coupling to gravity and eventually to other fields.
Alternatively, one can start with a \lq\lq dark energy fluid" obeying a given equation of state as a source of the field equations and study the resulting inflationary dynamics.
Such an approach has been developed, e.g., in Ref. \cite{chap}, where the inflaton field has been assumed to exhibit the same thermodynamic properties of a fluid obeying a Chaplygin gas-like equation of state.
In the present paper, we follow the same line of thinking as above to develop an inflationary model based on a dark energy field described by a Shan-Chen-like equation of state \cite{shan-chen,sc_prd}.
This equation of state has the suitable property to support a phase transition between low and high density regimes, both characterized by an ideal gas behavior, i.e., pressure and density change in linear proportion to each other.
It was first introduced by Shan and Chen in the context of lattice kinetic theory \cite{shan-chen}, and recently applied to a cosmological context in Ref. \cite{sc_prd} to model the growth of the dark energy component of the present universe.
In the sequel, we will show that this model satisfies current observational constraints over a wide range of parameters, and also provides a a graceful exit mechanism from the inflationary epoch.

\section{Scalar field inflationary models}

The action associated with a scalar field $\phi$ minimally coupled to gravity is given by
\beq
S=\int d^4x\sqrt{-{\rm g}}\left[\frac{M_{\rm pl}^2}{2}R-{\mathcal L}(X,\phi)\right]\,,
\eeq
where ${\rm g}$ is the determinant of the metric, $R$ is the Ricci scalar, $M_{\rm pl}=(8\pi G)^{-1/2}$ is the reduced Planck mass and  ${\mathcal L}$ is the Lagrangian density, which can be in general an arbitrary function of the field and its kinetic term $X=-\frac12g^{\mu\nu}\partial_\mu\phi\partial_\nu\phi$.

Variation of the action with respect to the metric leads to the energy momentum tensor, which can be cast in the form of a perfect fluid, with energy density and pressure given by \cite{dam_mukh}
\beq
\label{rhoandpgen}
\rho=2X{\mathcal L}_X-{\mathcal L}\,,\qquad
p={\mathcal L}\,,
\eeq
where the subscript $X$ indicates differentiation with respect to $X$.
The evolution of a scalar field in a given gravitational background is equivalently described by the motion of a hydrodynamic fluid with a given equation of state.
The hydrodynamic analogy proves useful even if the pressure cannot be expressed in terms of the density alone, because in general $\phi$ and $X$ are independent, as pointed out in Ref. \cite{dam_mukh}.

In the context of inflation, several models have been proposed by selecting a particular functional form of the Lagrangian density (see, e.g., Refs. \cite{dam_mukh,garr_mukh,dbi_pap,sahni}).
In the present paper, we discuss a canonical scalar field model, i.e., with ${\mathcal L}= X-V(\phi)$, where $X=\dot\phi^2/2$ is the standard kinetic term and $V$ the potential.
As usual in inflationary cosmology, we also assume the background gravitational field to be a FRW universe with vanishing spatial curvature, i.e., with metric $ds^2=-dt^2+a^2(dx^2+dy^2+dz^2)$, where $a=a(t)$ is the scale factor.
The Euler-Lagrange equations for this system read as follows
\begin{eqnarray}
\label{ELeqns}
H^2&=&\frac{1}{3M_{\rm pl}^2}\left(\frac{\dot\phi^2}{2}+V\right)\,,\nonumber\\
0&=&\ddot\phi+3H\dot\phi+V'\,,
\end{eqnarray}
where $H=\dot a/a$ is the Hubble parameter.
Here a overdot indicates derivative with respect to cosmic time $t$, whereas a prime denotes differentiation with respect to the scalar field $\phi$.
The hydrodynamic analog of this formulation consists then in taking a perfect fluid as a source of the Einstein's field equations, with energy density and pressure given by
\beq
\label{rhoandp}
\rho=\frac{\dot\phi^2}{2}+V\,,\qquad
p=\frac{\dot\phi^2}{2}-V\,,
\eeq
so that
\beq
\label{Vdef}
V=\frac12(\rho-p)\,,\qquad
\dot\phi^2=\rho+p\,.
\eeq
The field equations
\beq
\label{FRWeqs}
H^2=\frac{\rho}{3M_{\rm pl}^2}\,,\qquad
\dot\rho=-3H(\rho +p)\,,
\eeq
are then completely equivalent to Eqs.  (\ref{ELeqns}).

\subsection{Slow-roll inflation}

Let us consider a slow-roll approximation for the (background) scalar field, i.e., the case when the potential energy $V$ dominates over the kinetic energy ${\dot\phi^2}/{2}$, driving a quasi-exponential expansion of the universe.
The following conditions hold \cite{liddle}
\beq
\label{SLconds}
\ddot\phi\ll 3H\dot\phi\,,\qquad
\frac{\dot\phi^2}{2}\ll V\,,
\eeq
implying that
\beq
\label{SLconds2}
V'\approx-3H\dot\phi\,,\quad
H^2\approx\frac{V}{3M_{\rm pl}^2}\,,\quad
p\approx-\rho\,.
\eeq

In this case one defines the slow-roll parameters
\begin{eqnarray}
\label{PSRparams}
\epsilon&=&\frac12M_{\rm pl}^2\left(\frac{V'}{V}\right)^2\,,\nonumber\\
\eta&=&M_{\rm pl}^2\frac{V''}{V}\,,\nonumber\\
\Xi&=&M_{\rm pl}^4\frac{V'V'''}{V^2}\,,
\end{eqnarray}
which should remain small, i.e., $\epsilon\ll1$, $|\eta|\ll1$, $|\Xi|\ll1$.
Note that under these conditions $\dot H/H^2\approx-\epsilon$.

Inflation is commonly characterized by the number $N$ of $e$-folds of the expansion.
It is defined as the natural logarithm of the ratio of the scale factor at the final time $t_e$ to its value at some initial time, i.e.,
\beq
\label{eqN}
N=\int_t^{t_e}H dt=\ln\frac{a_e}{a}\,.
\eeq
This measures the amount of inflation that still has to occur after a time $t$, with $N$ decreasing to $0$ at the end of inflation.
When slow-roll is violated, i.e., $\epsilon(\phi_e)\approx1$ (or $|\eta(\phi_e)|\approx1$, $|\Xi(\phi_e)|\approx1$), the inflationary phase ends.
As it is well known, the universe should then be reheated, undergoing a transition to the radiative phase of the standard cosmological model.
The stability issue related to scalar perturbations of scalar field inflationary models in the slow-roll regime is briefly recalled in the Appendix.

In the following sections, we will develop a canonical scalar field model of inflation based on a dark energy field described by a suitable non-ideal equation of state supporting phase-transitions.

\section{The Shan-Chen fluid model}

Before discussing the application to inflationary cosmology, we shall review below the basic features of non-ideal fluids obeying a Shan-Chen-like (SC) equation of state \cite{shan-chen,sc_prd}, with special focus on the underlying microphysics and its relevance to cosmological models.

\subsection{Microscopic foundations}

Shan and Chen first used a non-ideal equation of state to model dynamic phase transitions in the context of lattice kinetic theory \cite{shan-chen}. The main motivation was to circumvent the problem of the very small time-steps imposed by the short-range (hard-core) repulsion of atomic potentials in the numerical integration
of the equations of motion of molecular fluids.
The distinctive feature of the SC equation of state is the replacement of hard-core repulsive interactions, which are needed to tame unstable density build-up, with a purely attractive force, with the peculiar property of becoming vanishingly small above a given density threshold, so as to prevent the onset of instabilities due to uncontrolled density pile-up.
Since high-density implies short spatial separation, the SC potential implements a form of effective of ``asymptotic freedom,'' meaning by this that molecules below a certain separation behave basically like free particles.
Since its inception, the SC method has met with major success for the numerical simulation
of a broad variety of complex flows with phase-transitions \cite{LB1,LB2}.

More in detail, with specific reference to {\it lattice} fluids, for which the time-step is fixed by the lattice size, Shan and Chen \cite{shan-chen} proposed a \lq\lq synthetic" repulsion-free potential of the form:
\beq
\label{SCPOT}
V({\mathbf x},{\mathbf x}')=\psi({\mathbf x})G({\mathbf x}-{\mathbf x}')\psi({\mathbf x}')\,,
\eeq
where the generalized density $\psi({\mathbf x}) = \psi[\rho({\mathbf x})]$ is a local functional
of the fluid density and $G({\mathbf x}-{\mathbf x}')$ is the Green function of the interaction.
In the above
\beq
{\mathbf x}'={\mathbf x}+{\mathbf e}_a\,,
\eeq
where ${\mathbf e}_a$ denotes a generic spatial direction in the lattice.
The explicit dependence on time of the various functions defined above has been omitted for notational simplicity.
For instance, a typical two-dimensional lattice features one rest particle ($|{\mathbf e}_0 |=0$), $4$ nearest-neighbors ($|{\mathbf e}_a | =c_L \Delta t$), and $4$ next-nearest-neighbors  ($|{\mathbf e}_a| =c_L \Delta t \sqrt 2)$, $c_L={\Delta x}/{\Delta t}$ being the lattice \lq\lq light speed."

Shan and Chen took $G({\mathbf x}-{\mathbf x}')={\mathcal G}$ for
$|{\mathbf e}_a |<c_L \Delta t \sqrt 2$ and zero elsewhere, where ${\mathcal G}<0$ codes
for attractive interaction.
The associated force per unit volume of the fluid reads as follows:
\begin{equation}
\label{SCFORCE}
{\mathbf F}({\mathbf x})=-\psi({\mathbf x}){\mathcal G}\sum_a\psi({\mathbf x}+{\mathbf e}_a){\mathbf e}_a\,,
\end{equation}
which equals $-{\mathcal G} c_s^2 \nabla \psi^2/2$ in the limit $\Delta t \to 0$.
Taylor expanding the above expression yields:
\begin{equation}
\label{Force_approx}
{\mathbf F}({\mathbf x}) = -{\mathcal G} \psi({\mathbf x}) \nabla \psi({\mathbf x}) + O(\Delta t^3)\,,
\end{equation}
where we have taken into account that $\sum_a{\mathbf e}_a^i=0$ and
$\sum_a{\mathbf e}_a^i{\mathbf e}_a^j= (c_L^2 \Delta t^2/3)\delta^{ij}$.

Higher order terms describe physical properties, such as surface tension, which play
a crucial role in the dynamics of complex fluids.
It is readily shown that the above force contributes an
excess pressure of the form (in lattice units $\Delta t = \Delta x = c_L =1$)
\begin{equation}
\label{pstar}
\frac{p}{c_s^2}-\rho = \frac{\mathcal G}2 \psi^2(\rho)\,,
\end{equation}
$c_s$ being the sound speed of the ideal fluid, typically $c_s^2=1/3$ in lattice units.

Note that for attractive interactions, i.e., ${\mathcal G}<0$, the excess pressure is negative, leading
to a Van der Waals-like loop for ${\mathcal G}$ sufficiently negative.
The functional form $\psi(\rho)$ was chosen in Ref. \cite{shan-chen} in such a way as
to realize a vapor-liquid coexistence curve, i.e.,
\begin{equation}
\psi(\rho)= \rho_0  \left(1-e^{-\frac{\rho}{\rho_0}}\right)\,,
\end{equation}
where $\rho_0$ is a reference density, above which \lq\lq asymptotic freedom" sets in.
The above expression delivers a phase transition at $\rho_c = \rho_0 \ln2$ and ${\mathcal G}<{\mathcal G}_c=-4$.
In the low density regime ($\rho \ll \rho_0$) $\psi \rightarrow \rho$ and the Shan-Chen equation of state (\ref{pstar}) reduces to $p/c_s^2 = \rho + {\mathcal G} \rho^2/2$, which be unstable in the high density regime.
Due to the saturation of $\psi$ for $\rho\gg\rho_0$, in the high-density
limit the equation of state delivers instead $p/c_s^2 = \rho + {\mathcal G} \rho_0^2/2$.
An interesting feature of the Shan-Chen equation of state is the fact of supporting
a negative pressure for ${\mathcal G}$ sufficiently below ${\mathcal G}_c$, jointly with a positive $c_s^2$.

Finally, it is worth noting that $\psi({\mathbf x})$ can also be interpreted as a scalar field, interacting
via gauge quanta, whose propagator is precisely $G({\mathbf x}-{\mathbf x}')$ in Eqs. (\ref{SCPOT})--(\ref{SCFORCE}).
In the standard version, such gauge quanta do not propagate beyond the first Brillouin
region, the one associated with the $8$ lattice connections described above.
More recent variants of the model also include longer-range interactions, implementing the
competition between short-range attraction and long-range repulsion, which permits to describe
the dynamics of highly complex fluids such as foams and emulsions  \cite{falcucci}.

\subsection{Application to cosmology}

The SC equation of state is particularly interesting for cosmological applications because of its flexibility, which
permits to represent a broad variety of cosmological fluids, from radiation to dark energy, through a
smooth variation of its free parameters (see Fig. \ref{fig:0}, for a simple illustration).
Furthermore, it supports phase transitions, so that different epochs in the evolution of the universe
can be described as a natural consequence of the SC fluid dynamic equations.

As an example of such flexibility, we have recently presented in Ref. \cite{sc_prd} a new class of cosmological models consisting of a FRW universe with a fluid source, obeying a SC-like equation of state of the form:
\begin{eqnarray}
\label{pscdef}
p&=&w_{\rm (in)}\rho_{\rm (crit),0}  \left[\frac{\rho}{\rho_{\rm (crit),0} }+\frac{g}{2} \psi^2\right]\,,\nonumber\\
\psi&=& 1-e^{-\alpha \frac{\rho}{\rho_{\rm (crit),0}}}\,,
\end{eqnarray}
where $\rho_{\rm (crit),0}=3H_0^2M_{\rm pl}^2$ is the present value of the critical density ($H_0$ denoting the Hubble constant) and the dimensionless quantities $w_{\rm (in)}$, $g \le 0$ and $\alpha\ge0$ are free parameters of the model.
Note that these three parameters respond to a well-defined physical
interpretation: $w_{\rm (in)}$ describes the nature of matter, ordinary (positive)
versus exotic (negative). The parameter $g$ measures the strength
of non-ideal interactions within the matter component.
Finally, $\alpha$ sets the ratio between the actual
critical density and the density above which the excess pressure saturates
to a constant value, a regime sometimes associated with asymptotic-freedom, as
it corresponds to a vanishing contribution of non-ideal forces
to the momentum budget of the fluid.

We have shown in Ref. \cite{sc_prd} that, starting from an ordinary equation of state at early times (e.g., satisfying the energy condition typical of a radiation-dominated universe), a cosmological FRW fluid obeying the SC equation of state naturally evolves towards a present-day universe with a suitable dark-energy component, as a consequence of the fluid evolution equations. In the sequel, we shall explore the possibility to develop an inflationary model based on a dark energy field described by a SC-like equation of state of the form (\ref{pscdef}).

\begin{figure}
\centering
\subfigure{\includegraphics[scale=0.2]{fig0a.eps}}
\hspace{5mm}
\subfigure{\includegraphics[scale=0.2]{fig0b.eps}}
\caption{
The behavior of the SC pressure $p$ given by Eq. (\ref{pscdef}) is shown as a function of $\rho$ in units of $\rho_{\rm(crit),0}$ for the choice of parameters $\alpha=1$, $g=-6$ and different values of $w_{\rm (in)}=1/3$ (left) and $w_{\rm (in)}=-1$ (right).
}
\label{fig:0}
\end{figure}

\section{Shan-Chen inflation}

Let us turn to the scalar field formulation of inflation briefly recalled in Section II, assuming that the scalar field be described by a fluid satisfying the non-ideal Shan-Chen-like equation of state (\ref{pscdef}).
It proves convenient to introduce the following set of dimensionless variables:
\beq
\xi=\frac{\rho}{\rho_{\rm (crit),0}}\,, \qquad
x=\frac{a}{a_0}\,, \qquad
\tau=H_0t\,,
\eeq
so that for an expanding universe ($H>0$) Eqs. (\ref{FRWeqs}) reduce to
\beq
\label{FRWeqs2}
\frac{dx}{d\tau }=x\sqrt{\xi}\,,\qquad
\frac{d\xi}{d\tau }=-3\sqrt{\xi}[\xi +w_{\rm (in)}{\mathcal P}(\xi)]\,,
\eeq
where
\beq
\label{mathP}
{\mathcal P}(\xi)=\xi +\frac12 g \left(1-e^{-\alpha \xi }\right)^2\,.
\eeq
Besides the trivial solution $\xi=0=x$, the above system admits as fixed points the solutions of the following equation:
\beq
\label{attractor}
\xi_* +w_{\rm (in)}{\mathcal P}(\xi_*)=0\,,
\eeq
which can be at most two, for fixed values of $\alpha$ and $g$, as discussed in Ref. \cite{sc_prd}.

Note that Eq. (\ref{mathP}) reduces to the ideal gas expression ${\mathcal P}(\xi) \sim \xi$  in the
low-density limit $\alpha \xi \to 0$, while in the opposite high-density limit, it delivers
${\mathcal P} \sim \xi + \frac 12 g$, i.e., the non-ideal gas contribution reduces to a
constant, often associated with vacuum fluctuations.
For more details on the SC thermodynamics, see Ref. \cite{sc_prd}.
Here, we simply note that by changing the three parameters at hand, i.e., $w_{\rm (in)}$, $g$ and $\alpha$,
the SC equation of state can attain a broad range of values of
cosmological interest for the parameter $w_{\rm eff} \equiv p/\rho$.
Its behavior as a function of $\xi$ is shown in Fig. \ref{fig:1} for fixed values of $w_{\rm (in)}$ and $g$ and different values of $\alpha$.
Changing the value of $w_{\rm (in)}$ permits to obtain different low-density asymptotic regimes.
Increasing the value of $|g|$ implies that the relative maxima attain larger values.
Direct inspection of this plot shows that there exist values of $\alpha$ such that the SC equation of state undergoes a transition from exotic matter ($w_{\rm eff}<0$) to ordinary matter ($w_{\rm eff}>0$).

\begin{figure}
\begin{center}
\includegraphics[scale=0.35]{fig1.eps}
\end{center}
\caption{
The behavior of the ratio $w_{\rm eff}\equiv p/\rho$ as a function of $\xi$ is shown for the choice of parameters $w_{\rm (in)}=-1$, $g=-4$ and different values of $\alpha=[1,2,3]$.
The dashed curve (with $\alpha=2$) corresponds to the set of parameters used below for the numerical integration of the model equations.
}
\label{fig:1}
\end{figure}

According to the scalar field description discussed above, Eq. (\ref{Vdef}) implies that the
potential associated with the SC energy density and pressure is given by:
\beq
\label{potdef}
\frac{V}{\rho_{\rm (crit),0}}=\frac12\left(\xi-w_{\rm (in)}{\mathcal P}\right)\,,
\eeq
and the evolution equation for the dimensionless scalar field $\widetilde\phi=\phi/M_{\rm pl}$ reads as:
\beq
\label{eqphi}
\frac{d{\widetilde\phi}}{d\tau}=\sqrt{3(\xi+w_{\rm (in)}{\mathcal P})}\,.
\eeq
The slow-roll parameters (\ref{PSRparams}) turn out to be
\begin{eqnarray}
\label{PSRparams2}
\epsilon&=&\frac{3}{2}\frac{\xi(\xi+w_{\rm (in)}{\mathcal P})}{(\xi-w_{\rm (in)}{\mathcal P})^2}[1-w_{\rm (in)}+g\alpha w_{\rm (in)}\psi(\psi-1)]^2\,,\nonumber\\
\eta&=&-\frac{3}{4(\xi-w_{\rm (in)}{\mathcal P})}\sum_{k=0}^{4}A_k\psi^k\,,\nonumber\\
\Xi&=&\frac{9}{2}\frac{\xi(\xi+w_{\rm (in)}{\mathcal P})[1-w_{\rm (in)}+g\alpha w_{\rm (in)}\psi(\psi-1)]}{(\xi-w_{\rm (in)}{\mathcal P})^2}\nonumber\\
&&\times\sum_{k=0}^{4}B_k\psi^k\,,
\end{eqnarray}
where $\psi=1-e^{-\alpha\xi}$ is defined in Eq. (\ref{pscdef}), and
\begin{eqnarray}
A_0&=&4\xi(1+w_{\rm (in)})(\xi\alpha^2 gw_{\rm (in)}+w_{\rm (in)}-1)\,,\nonumber\\
A_1&=&2\xi gw_{\rm (in)}\alpha[3w_{\rm (in)}+1-6\alpha\xi(w_{\rm (in)}+1)]\,,\nonumber\\
A_2&=&gw_{\rm (in)}\left[8\alpha^2\xi^2(1+w_{\rm (in)})+w_{\rm (in)}-1\right.\nonumber\\
&&\left.
+2\alpha\xi\left(2\alpha gw_{\rm (in)}-3w_{\rm (in)}-1\right)\right]\,,\nonumber\\
A_3&=&-\alpha g^2w_{\rm (in)}^2(10\alpha\xi-1)\,,\nonumber\\
A_4&=&\alpha g^2w_{\rm (in)}^2(6\alpha\xi-1)\,.
\end{eqnarray}
and
\begin{eqnarray}
B_0&=&2(1-w_{\rm (in)}^2)-g\alpha^2w_{\rm (in)}\xi(5+7w_{\rm (in)})\nonumber\\
&&+6(1+w_{\rm (in)})g\alpha^3w_{\rm (in)}\xi^2\,,\nonumber\\
B_1&=&-4g\alpha w_{\rm (in)}^2+g\alpha^2w_{\rm (in)}\xi(21w_{\rm (in)}-4g\alpha w_{\rm (in)}+15)\nonumber\\
&&-14(1+w_{\rm (in)})g\alpha^3w_{\rm (in)}\xi^2\,,\nonumber\\
B_2&=&4g\alpha w_{\rm (in)}^2-\frac72g^2\alpha^2w_{\rm (in)}^2+8(1+w_{\rm (in)})g\alpha^3w_{\rm (in)}\xi^2\nonumber\\
&&-g\alpha^2w_{\rm (in)}\xi(10-19g\alpha w_{\rm (in)}+14w_{\rm (in)})\,,\nonumber\\
B_3&=&g^2\alpha^2w_{\rm (in)}^2\left(\frac{17}{2}-27\alpha\xi\right)\,,\nonumber\\
B_4&=&g^2\alpha^2w_{\rm (in)}^2(12\alpha\xi-5)\,.
\end{eqnarray}

Next, we study the behaviors of $V$, $\epsilon$, $\eta$ and $\Xi$ as functions of $\xi$ for fixed values of the parameters.
Approaching the initial singularity, $\xi$ goes to infinity or to a value of equilibrium ($\xi_*$).
In the former case we obtain:
\beq
\lim_{\xi\to\infty}\frac{V}{\rho_{\rm (crit),0}}=-\frac14w_{\rm (in)}g+\frac{\xi}{2}(1-w_{\rm (in)})\,,
\eeq
and
\begin{eqnarray}
\lim_{\xi\to\infty}\epsilon&=&\frac32(1+w_{\rm (in)})\,,\qquad
\lim_{\xi\to\infty}\eta=3(1+w_{\rm (in)})\,,\nonumber\\
\lim_{\xi\to\infty}\Xi&=&9(1+w_{\rm (in)})^2\,.
\end{eqnarray}
When $\xi\to\xi_*$ we have instead that $\epsilon\to0$ and $\Xi\to0$, whereas $\eta\to\eta(\xi_*)\equiv\eta_*$, with $\xi_*$ satisfying Eq. (\ref{attractor}).
The fixed points $\xi_*$ are inflationary attractors, corresponding to an exponential inflation, i.e.,
\beq
\frac{H_*^2}{H_0^2}=\xi_*\,,\qquad
x=e^{\sqrt{\xi_*}\tau}\,,
\eeq
as follows from Eqs. (\ref{FRWeqs}).

For completeness, at $\xi=0$ the potential behaves as
\beq
\lim_{\xi\to0}\frac{V}{\rho_{\rm (crit),0}}=\frac{\xi}{2}(1-w_{\rm (in)})\,,
\eeq
whereas the slow-roll parameters $\epsilon$, $\eta$ and $\Xi$ all approach the same values as in the limit $\xi\to\infty$ shown above.

\subsection{Observational constraints}

In the context of slow-roll inflation, the parameters (\ref{PSRparams}) plus the amplitude of the potential are sufficient to determine the observable quantities.
For instance, the ratio of tensor to scalar perturbations, the scalar spectral index and its running exponent are given by:
\begin{eqnarray}
r&=&16\epsilon\,,\nonumber\\
n_{s}&=&1-6\epsilon+2\eta\,,\nonumber\\
\alpha_{s}&\equiv&\frac{dn_{s}}{d \ln k}=16\epsilon\eta-24\epsilon^2-2\Xi\,,
\end{eqnarray}
respectively.
Recent cosmic microwave background data from Planck \cite{planck}, combined with the large angle polarization data from the Wilkinson Microwave Anisotropy Probe (WMAP) \cite{wmap} impose strong bounds on these parameters: $r<0.11$ and $n_{s}=0.9603\pm0.0073$ at $95\%$ confidence level. Furthermore, Planck data do not indicate any statistically significant running of the spectral index, i.e., $\alpha_{s}=-0.0134\pm0.0090$.
Finally, the combination of the very recent results of BICEP2 \cite{bicep2} with the other experiments favors a value of the tensor-to-scalar ratio $r$ between $0.13$ and $0.25$ (with $0.2$ preferred).

\subsection{Results}

In order to study the implications of observational constraints on the SC potential and the free parameters of the model, we have first to check that the slow-roll conditions are fulfilled.
Inflation ends if/when $\epsilon\approx1$ (or $|\eta|\approx1$, $|\Xi|\approx1$).
This condition fixes the value of the field $\widetilde\phi_e$ at the end of inflation.
Next, the potential must allow for a sufficient number of inflationary $e-$folds between horizon crossing for observable scales and the end of inflation, which is typically about 60.
Requiring that $N_i\approx60$ at the beginning of inflation provides a condition on the initial value $\widetilde\phi_i$ of the field in order to obtain a sufficient number of $e-$folds, which is assumed to be $N_e=0$ at the end of inflation (with $\widetilde\phi_e=0$ too).

It is convenient to express the evolution of the scalar field $\widetilde\phi$ and the number of $e-$folds $N$ in terms of $\xi$ as follows:
\begin{eqnarray}
\label{eqsNphi}
\frac{d\widetilde\phi}{d\xi}&=& -\frac1{\sqrt{3\xi(\xi+w_{\rm (in)}{\mathcal P})}}\,,\nonumber\\
\frac{dN}{d\xi}&=& \frac1{3(\xi+w_{\rm (in)}{\mathcal P})}\,,
\end{eqnarray}
from Eqs. (\ref{eqN}) and (\ref{eqphi}).
Since in the limit of  both high and low density the SC equation of state reduces to $p\sim w_{\rm (in)}\rho$, we assume hereafter $w_{\rm (in)}=-1$, to match the inflationary condition also in these asymptotic regimes.
This choice allows for an analytical study of the model equations.

In fact, the field equations (\ref{FRWeqs2}) reduce to
\beq
\label{FRWeqs3}
\frac{dx}{d\tau }=x\sqrt{\xi}\,,\qquad
\frac{d\xi}{d\tau }=\frac32g\sqrt{\xi}(1-e^{-\beta})^2\,.
\eeq
The latter equation can be also written as
\beq
\frac{d\beta}{dx }=-\frac1{\sigma^2x}(1-e^{-\beta})^2\,,
\eeq
in terms of $\beta=\alpha\xi$ and the new parameter $\sigma^2=2/(3\alpha|g|)$ which summarizes the whole dependence on the parameters of the model.
The solution is
\beq
\beta=\ln\left(1+\frac1y\right)\,,\qquad
y=W(x^{1/\sigma^2}e^{C/\sigma^2})\,,
\eeq
where $W(z)$ denotes the Lambert $W$ function (see, e.g., Ref. \cite{corless} for its definition and main properties) and $C$ is an integration constant.
Upon inverting we obtain
\beq
x=e^{-\sigma^2\beta}(1-e^{-\beta})^{-\sigma^2}e^{-C+\sigma^2/(1-e^{-\beta})}\,.
\eeq

Eqs. (\ref{eqsNphi}) then become
\begin{eqnarray}
\label{eqsNphi2}
\frac{d\widetilde\phi}{d\beta}&=& -\frac{\sigma}{\sqrt{\beta}(1-e^{-\beta})}\,,\nonumber\\
\frac{dN}{d\beta}&=& \frac{\sigma^2}{(1-e^{-\beta})^2}\,.
\end{eqnarray}
The solution for $N$ is straightforward
\beq
\label{solN}
N-N_0= \sigma^2\left[\beta-\frac1{1-e^{-\beta}}+\ln(1-e^{-\beta})\right]\,.
\eeq
The solution for $\widetilde\phi$ instead can only be given formally, i.e.,
\beq
\label{solphi}
\widetilde\phi-\widetilde\phi_0=-\sigma\sum_{k=0}^{\infty}\sqrt{\frac{\pi}{k}}{\rm erf}(\sqrt{k\beta})\,,
\eeq
where ${\rm erf}(z)$ denotes the error function and the term $k=0$ is taken as a limit.
We have used here the geometric series representation for $(1-e^{-\beta})^{-1}$, whose convergence is ensured for $\beta\gg 1$.
The quantities $N_0$ and $\widetilde\phi_0$ in Eqs. (\ref{solN}) and (\ref{solphi}) are integration constants.

The potential (\ref{potdef}) in this case becomes
\beq
\frac{\alpha V}{\rho_{\rm (crit),0}}=\beta-\frac1{6\sigma^2}\psi^2\,,
\eeq
and the slow-roll parameters (\ref{PSRparams2}) take the following compact form:
\begin{eqnarray}
\epsilon&=&
2\psi^2\beta\frac{(3\sigma^2-\psi+\psi^2)^2}{\sigma^2(-6\beta\sigma^2+\psi^2)^2}\,,\nonumber\\
\eta&=&\frac{\psi}{\sigma^2(-6\beta\sigma^2+\psi^2)}[(6\beta-1)\psi^3+(1-10\beta)\psi^2\nonumber\\
&&
+(6\beta\sigma^2+4\beta-3\sigma^2)\psi-6\beta\sigma^2]\,,\nonumber\\
\Xi&=&-\frac{2(1-\psi)(3\sigma^2-\psi+\psi^2)\psi^2\beta}{\sigma^4(-6\beta\sigma^2+\psi^2)^2}
[2(12\beta-5)\psi^3\nonumber\\
&&
+(7-30\beta)\psi^2+4(3\beta\sigma^2+2\beta-3\sigma^2)\psi-6\beta\sigma^2]\,,\nonumber\\
\end{eqnarray}
where $\psi=1-e^{-\beta}$ as from Eq. (\ref{pscdef}).
Fig. \ref{fig:2} shows the boundary of the region in the parameter space $(\beta,\alpha|g|)$ where the slow-roll regime holds.
The asymptotic behavior of the potential for large values of $\beta$ is then $V\sim\beta$.
In this limit, from Eq. (\ref{eqsNphi2}), one also has $\widetilde\phi\sim\sqrt{\beta}$, implying that $V\sim\widetilde\phi^2$.

\begin{figure}
\begin{center}
\includegraphics[scale=0.32]{fig2.eps}
\end{center}
\caption{
The curves $\epsilon=1$, $\eta=1$ and $\Xi=1$ are implicitly plotted as functions of $\alpha|g|$ and $\beta$ for $w_{\rm (in)}=-1$.
The slow-roll regime turns out to be valid in the region below each curve.
}
\label{fig:2}
\end{figure}

Let us turn to the general equations (\ref{eqsNphi}).
An example of numerical integration is shown in Fig. \ref{fig:3} for the choice of SC parameters $w_{\rm (in)}=-1$, $g=-4$ and $\alpha=2$.
Fig. \ref{fig:3} (a) shows the behavior of the potential $V$ as a function of $\phi$.
It starts from a large value and monotonically decreases towards a minimum non-zero value, typical of hybrid models \cite{dodelson}.
In Fig. \ref{fig:3} (b), we plot the slow-roll parameters associated with the SC potential. The slow-roll regime ends due to $\epsilon$, which first approaches unity.
Fig. \ref{fig:3} (c) shows the number of $e-$folds during the inflation matching the interval $N\approx[0,60]$ commonly assumed in inflationary models.
Finally, in Fig. \ref{fig:3} (d) we show the existence of a graceful exit mechanism from inflation by plotting as a function of $\phi$ the parameter $w_{\rm eff}$, i.e., the ratio between energy density and pressure.
With the above choice of SC parameters, we obtain $r\approx0.13$, $n_{s}\approx0.97$ and $\alpha_{s}\approx-5\times10^{-4}$, which are in agreement with observational data.
Fig. \ref{fig:4} shows the agreement of our analysis with the joint constraints (at $1\sigma$ and  $2\sigma$ confidence level) on $n_s$ versus $r$ from current Planck+WP+highL+BICEP2 data (see Ref. \cite{bicep2} and references therein).

\begin{figure}
\centering
\subfigure[]{\includegraphics[scale=0.2]{fig3a.eps}}
\hspace{5mm}
\subfigure[]{\includegraphics[scale=0.2]{fig3b.eps}}\\[1cm]
\subfigure[]{\includegraphics[scale=0.2]{fig3c.eps}}
\hspace{5mm}
\subfigure[]{\includegraphics[scale=0.2]{fig3d.eps}}
\caption{
The model equations (\ref{eqsNphi}) are numerically integrated for the choice of parameters $w_{\rm (in)}=-1$, $g=-4$ and $\alpha=2$.
The behavior of the potential $V$ (in units of $\rho_{\rm (crit),0}$), the slow-roll parameters $\epsilon$, $\eta$ and $\Xi$, the number of $e-$folds $N$ during inflation and the ratio $p/\rho\equiv w_{\rm eff}$ between energy density and pressure as functions of $\phi$ (in units of $M_{\rm pl}$) is shown in panels (a) to (d), respectively.
}
\label{fig:3}
\end{figure}

\begin{figure}
\begin{center}
\includegraphics[scale=0.4]{fig4.eps}
\end{center}
\caption{
The contours of the ratio of tensor to scalar perturbations $r$ versus the scalar spectral index $n_s$ are {\it qualitatively} drawn from Planck+WP+highL+BICEP2 data \cite{bicep2}.
The straight line shows how $r$ changes as a function of $n_s$ for a SC model with the same choice of parameters as in Fig. \ref{fig:3}.
Noticeably, the same behavior is kept for a wide range of SC parameters $\alpha$ and $g$ that we have explored.
}
\label{fig:4}
\end{figure}

\section{Concluding remarks}

Summarizing, we have proposed a scalar field model for inflation based on the
hydrodynamic analog of a Shan-Chen-like fluid.
A SC-like equation of state has been recently introduced in cosmology to represent the current distribution of dark energy, based on its property of evolving ordinary matter into a matter-energy component with an equation of state $p\approx-\rho$,
through a phase transition mechanism.
In the context of inflation, we have considered a flat FRW universe filled by a canonical scalar field, with kinetic energy and potential related to   the SC energy density and pressure.
The evolution of the scalar field is thus completely determined by the SC dynamics, and we have analyzed in detail its properties in the slow-roll approximation.
Numerical inspection of the associated equations shows that simple choices of the free parameters of the SC model are consistent with current Planck, WMAP and BICEP2 data, i.e., the minimal viability requrement for any cosmological model.
Furthermore, the equation of state undergoes a transition between $p/\rho<0$ (exotic matter) during inflation to $p/\rho>0$ (ordinary matter) at late times, thus
providing also a graceful exit mechanism.
A more refined choice of parameters, as well as a suitable extension of the SC model presented here, are expected to match further available data.
Future directions of investigation will focus on the effects of
quantum fluctuations on the Shan-Chen cosmology and their
potential connections with the theory of hydrodynamic turbulence
\cite{ESS}.

redpajama_set_name: RedPajamaArXiv


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text:
Q: SQL Server 2005 query optimization with Max subquery I've got a table that looks like this (I wasn't sure what all might be relevant, so I had Toad dump the whole structure)
CREATE TABLE [dbo].[TScore] (
[CustomerID] int NOT NULL,
[ApplNo] numeric(18, 0) NOT NULL,
[BScore] int NULL,
[OrigAmt] money NULL,
[MaxAmt] money NULL,
[DateCreated] datetime NULL,
[UserCreated] char(8) NULL,
[DateModified] datetime NULL,
[UserModified] char(8) NULL,
CONSTRAINT [PK_TScore]
PRIMARY KEY CLUSTERED ([CustomerID] ASC, [ApplNo] ASC)
);

And when I run the following query (on a database with 3 million records in the TScore table) it takes about a second to run, even though if I just do: Select BScore from CustomerDB..TScore WHERE CustomerID = 12345, it is instant (and only returns 10 records) -- seems like there should be some efficient way to do the Max(ApplNo) effect in a single query, but I'm a relative noob to SQL Server, and not sure -- I'm thinking I may need a separate key for ApplNo, but not sure how clustered keys work.
SELECT BScore
FROM CustomerDB..TScore (NOLOCK)
WHERE ApplNo = (SELECT Max(ApplNo)
               FROM CustomerDB..TScore sc2 (NOLOCK)
               WHERE sc2.CustomerID = 12345)

Thanks much for any tips (pointers on where to look for optimization of sql server stuff appreciated as well)

A: When you filter by ApplNo, you are using only part of the key. And not the left hand side. This means the index has be scanned (look at all rows) not seeked (drill to a row) to find the values.

*

*If you are looking for ApplNo values for the same CustomerID:

Quick way. Use the full clustered index:
SELECT BScore
FROM CustomerDB..TScore
WHERE ApplNo = (SELECT Max(ApplNo)
               FROM CustomerDB..TScore sc2
               WHERE sc2.CustomerID = 12345)
AND CustomerID = 12345

This can be changed into a JOIN
SELECT BScore
FROM
     CustomerDB..TScore T1
     JOIN
     (SELECT Max(ApplNo) AS MaxApplNo, CustomerID
      FROM CustomerDB..TScore sc2
      WHERE sc2.CustomerID = 12345
     ) T2 ON T1.CustomerID = T2.CustomerID AND T1.ApplNo= T2.MaxApplNo

*

*If you are looking for ApplNo values independent of CustomerID, then I'd look at a separate index. This matches your intent of the current code

CREATE INDEX IX_ApplNo ON TScore (ApplNo) INCLUDE (BScore);
Reversing the key order won't help because then your WHERE sc2.CustomerID = 12345 will scan, not seek
Note: using NOLOCK everywhere is a bad practice


text:
BUSINESS HONOREE ― JOSEPH PULITZER
Joseph Pulitzer medal designed by Eugene Daub, struck by Medallic Art Company in quantities of 110 bronze, 63 pure silver, and 34 gold-plated silver. Obverse: Portrait, JOSEPH PULITZER 1847-1911, DAUB. Reverse: Standing figure of Pulitzer, OUR REPUBLIC AND ITS PRESS WILL RISE OR FALL TOGETHER, DAUB. 49 x 47 mm.
Joseph Pulitzer was born in Mako, Hungary on April 10, 1847. Both his parents were registered by the official Jewish registry under the heading of Religion as "Israelitic" and under Nationality as "Jewish." In accordance with Jewish law, Joseph Pulitzer was circumcised eight days after his birth, and he likely received a traditional Jewish upbringing at Mako's cheder (Jewish primary school).
Joseph Pulitzer arrived in Boston from Hungary in 1864 at the age of 17, his passage having been paid by Massachusetts military recruiters who were seeking soldiers for the American Civil War. Pulitzer was a part of Sheridan's troopers, in the First New York Lincoln Cavalry in Company L., where he served for eight months.
On March 6, 1867, Pulitzer became an American citizen, and just two years later he won a seat in the St. Louis state legislature as a Republican. In 1884, Pulitzer was elected to the U.S. House of Representatives from New York as a Democrat. He served from March 4, 1885 until April 10, 1886, resigning due to the pressure of journalistic duties.
In 1879, Joseph Pulitzer bought both the St. Louis Dispatch and the St. Louis Post, merging the two papers as the St. Louis Post-Dispatch. With his own paper, Pulitzer developed his role as a champion of the common man, featuring exposés and a hard-hitting populist approach.
Putting aside serious health concerns, in 1883 Pulitzer negotiated the purchase of The New York World, which was in financial straits. Charles Dana, the editor of the rival New York Sun, attacked Pulitzer in print, using derogatory terms like "Judas Pulitzer." Pulitzer crusaded against public and private corruption, filled the news columns with a spate of sensationalized features, made the first extensive use of illustrations, and staged news stunts. In one of the most successful promotions, The World raised public subscriptions for the building of a pedestal at the entrance to the New York harbor so that the Statue of Liberty, which was stranded in France awaiting shipment, could be emplaced.
From 1896 to 1898, Pulitzer was in a bitter circulation battle with William Randolph Hearst's Journal, in which there were no apparent restraints on sensationalism or fabrication of news. When the Cubans rebelled against Spanish rule, Pulitzer and Hearst both called for war against Spain after the U.S. battleship Maine mysteriously blew up and sank in Havana harbor on February 15, 1898. Congress reacted to the outcry with a war resolution. After the four-month war, Pulitzer withdrew from what had become known as "yellow journalism," and The World became more restrained. Pulitzer waged courageous and often successful crusades against corrupt practices in government and business. He was responsible to a large extent for passage of antitrust legislation and regulation of the insurance industry.
In May 1904, writing in The North American Review in support of his proposal for the founding of a school of journalism, Pulitzer summarized his credo: "Our Republic and its press will rise or fall together. An able, disinterested, public-spirited press, with trained intelligence to know the right and courage to do it, can preserve that public virtue without which popular government is a sham and a mockery. A cynical, mercenary, demagogic press will produce in time a people as base as itself. The power to mould the future of the Republic will be in the hands of the journalists of future generations."
The Pulitzer Prizes were established in 1917 by money bequeathed by Joseph Pulitzer to Columbia University to recognize artistic and journalistic achievements in the United States. The prizes are given annually to award achievements in American journalism and photography, as well as literature and history, poetry, music and drama. The Columbia School of Journalism opened in 1912, thanks to Pulitzer's philanthropic bequest. Jewish Americans have won Pulitzer Prizes in many categories. Some of the winners in fiction include Bernard Melamud, Philip Roth, Neil Simon, Art Spiegelman, and Herman Wouk. Pulitzer winning Jewish American playwrights and musicians include Ira Gershwin, George S. Kaufman, Marvin Hamlisch, Arthur Miller, Richard Rodgers, Stephen Sondheim, and Wendy Wasserstein.
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