Log Helioter **************************************************************** Medii 3 orare: - se incarca cu Open fisierul 'sAN.txt'. Atentie: se inlocuiesc primele valoari pt vit, dens, temp (daca sunt invalide) cu ultimile valori din anul precedent si de asemenea ultimile valori (daca sunt invalide) pe acel an cu ultimile valori valide. - click 'Medii3Orare'. Se creaza fisierul '3m-an.dat' care contine mediile 3h pe anul respectiv. Ultimele 3 coloane sunt: viteza, densitate si temperatura plasmei. Primul pas este interpolarea datelor lipsa cu ajutorul functiei 'interpolareFct' iar al doilea pas este calcularea mediilor triorare cu ajutorul functiei 'TRIhFct' care genereaza fisierul '3m-an.dat' - 'Open' - '3m-an.dat' - 'PlotNVT' - vizualizarea suprapusa a graficelor vitezei, densitatii si temp plasmei in functie de luna selectata + fisier 'ps' - 'PlotNVT-3x' - vizualizarea in coloana a celor 3 grafice + fisier 'ps' Bug: cand avem an bisect se schimba NDays=366 in 'medii3Orare.pro' **************************************************************** Drepte regresie - Vpr & Npr - Am creat un fisier txt 'input-regresie-10.04.2005-12.06.2005-V_Npr-txt' care contine urmatoarele coloane pt perioada de 2 luni de date fara gapuri: Nr. Nomni2 Vomni2 Nsoho Vsoho - open; incarc fisierul sursa 'input...'; variabila 'catalog.sav' isi schimba forma - Dr.Reg. -> accesez fct 'dreaptaReg' din fisierul 'dataFct.pro' care imi creaza dreapta de regresie Vomni2 versus Vsoho (output 'ps'). daca se doreste si dreapta de regresie a densitatii protonilor se schimba valoare variabilei de selectie 'selectDrReg=1'. In acest caz, se afiseaza grafic dreapta de regresie pt densitate si se genereaza 2 fisiere 'ps' - daca se ruleaza din nou programul nu mai trebuie incarcat fisierul input. Continutul variabilei 'catalog.sav' nu s-a modificat. **************************************************************** Find-Gap -> determinarea intervalelor datelor lipsa - open; selectie 'omni2_an.dat' - readOmni2; output sAN.txt - open; selectie sAN.txt - Find-Gap ; se afiseaza intervalul (>1zi) datelor lipsa Daca se doreste reafisarea intervalului: - open; selectie sAN.txt ; atat timp cat sAN.txt nu a fost modificat - Find-Gap ; se afiseaza intervalul (>1zi) datelor lipsa **************************************************************** log prelucrat Catalog versiunea catalogMain10 1) se incarca un fisier de tip 'omni2_an.dat' folosind butonul 'Open' si se creaza o structura de data de tip 'catalog.sav'; aceasta structura poate fi apelata de celelalte functii ale programului. 2) construit fisier cu date extrase din 'omni2_an.dat' intr-un fisier 'sAn.txt' care contine numai urmatoarele coloane: An Luna Ziua Ora Rot_B Ziua_B ID-sp Pr-D Pr-sp Pr-T Acest fisier este creat de butonul ReadOmni2 folosind strct. 'catalog.sav' creat in primul pas din fisiere 'omni2_an.dat' 3) creat un fisier de tip '3m-an.dat' cu ajutorul butonului Omni2-M. Fisierul primeste ca intrare 'sAn.txt' si genereaza 5 fisiere printre care si fisierul '3m-an.dat'. Inainte de rularea prg. se schimba urmatorii parametrii: anul procesat, nr de zile Ndays (difera la anii bisecti); de asemenea se verifica ca prima si ultima valoare a vitezei plasmei din fisierul 'sAn.txt' sa fie valida, altfel prg. da eroare daca prima valoare lipseste sau nu calculeaza ultimile medii triorare daca ultima valoare lipseste 4) se foloseste din nou butonul 'Open' pt a citii fisierul '3m-an.dat' si a schimba valoarea structurii de date 'catalog.sav'. 5) acum se poate folosii butonul 'PlotV' pt a vedea datele pe anul respectiv grupate pe luni; se poate citii cu mouse-ul valorile pct-lor de pe grafic; se poate genera folosind butonul 'PS' un fisier post scriptul care contine graficul selectat. ******************************************* Pasi grafice triorare Omni2 (Vprotoni/timp) pe ani: - descarc omni2-73.dat - din acest fisier trebuisc extrase urmatoarele date: Date: year luna ziua ora BartelsRotationNumber Bartels_Day ID-SW_plasma_spacecraft Proton_Density Plasma(Bulk)_speed Proton_Temperature Col. no: 1 deCal. deCal. 3 4 deCal(1-27) 6 24 (N/cm^3) 25 (km/s) 23 cu ajutorul excelului. se creaza un fisier sAn.txt (ex: s1973.txt) cu tab-ul delimitator intre coloane. - se executa fisierul omni19**_3m.pro (IDL) pt a genera mediile triorare; daca apare o eroare legata de scris element matrice superior se corecteaza primele 3 date ale vitezei protonilor; programul are input s19**.txt si output: 3m-19*.dat - se deschide fisierul 3m-1973.dat in excel si se constuisc graficele V(km/s) in functie de timp pentru fiecare luna. se construieste o axa x (vezi fisiere vechi 3m-19*-ver** -> excel worksheet) Legenda: - High-Speed Plasma Stream - HSPS = a large increase in the solar wind velocity lasting for several days. Lindblad & Lundstedt -> the difference between the smallest 3-hr velocity value for a given day and the largest 3-hr value of the following day. If this difference is greater than 100 km/s => a possible HSPS. A second criteria for a HSPS is an observable increase in the ion density immediately preceding the stream and/or a rapidly varying magnetic field. - Bartel rotation number = The serial number assigned to 27-day recurrence periods of solar and geophysical parameters. The equatorial rotation rate of the Sun is very close to 27 days. Rotation 1 Day 1 in this sequence was assigned arbitrarily by J. Bartels to February 8, 1832. - POL IMF (+/-) = the dominant polarity of the interplanetary magnetic field for the duration of the stream - V0 = pre-stream velocity; Vm = peak velocity of the HSPS - DV0 = the velocity increase between 2 consecutive days - DVm = the difference between Vm and V0 - corotating stream = is emitted from a coronal hole and is characterized by: a peak in the proton density (n) beginning several hours before the increase in velocity. A sharp decrese of n during the velocity increase. The magnetic field (B) shows a peak starting with the compressive phase of the density enhancement and terminating at the end of the velocity increase. The proton temp. (T) increase with velocity and tends to follow the temporal variations of the velocity (v) - flare associated stream = is characterized by simultaneous increases in V, n, B and T. The plasma parameters V,n, and B show large fluctuations during the maximum velocity phase. The field polarity shows inversions and irregularities. - K, Kp, and ap Indices The K-index is quasi-logarithmic local index of the 3-hourly range in magnetic activity relative to an assumed quiet-day curve for a single geomagnetic observatory site. First introduced by J. Bartels in 1938, it consists of a single-digit 0 thru 9 for each 3-hour interval of the universal time day (UT). The planetary 3-hour-range index Kp is the mean standardized K-index from 13 geomagnetic observatories between 44 degrees and 60 degrees northern or southern geomagnetic latitude. The scale is O to 9 expressed in thirds of a unit, e.g. 5- is 4 2/3, 5 is 5 and 5+ is 5 1/3. This planetary index is designed to measure solar particle radiation by its magnetic effects. The 3-hourly ap (equivalent range) index is derived from the Kp index as follows: Kp = 0o 0+ 1- 1o 1+ 2- 2o 2+ 3- 3o 3+ 4- 4o 4+ ap = 0 2 3 4 5 6 7 9 12 15 18 22 27 32 Kp = 5- 5o 5+ 6- 6o 6+ 7- 7o 7+ 8- 8o 8+ 9- 9o ap = 39 48 56 67 80 94 111 132 154 179 207 236 300 400 Other planetary indices include the Ap* and AA*. The Ap* index is defined as the earliest occurring maximum 24-hour value obtained by computing an 8-point running average of successive 3-hour ap indices during a geomagnetic storm event and is uniquely associated with the storm event. The AA* index is similar to the Ap* index, but has a longer history and is based on reports from only two stations.