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Flare, solar wind, and CME (Coronal Mass Ejection) are complex Sun activities. A solar flare is a violent explosion in the Sun, resulted from the sudden release of energy stored in the magnetic fields because of the magnetic reconnection. CME are huge bubbles of gas ejected and plasma consisting pri...

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Main Author: NENG RAHAYU (NIM 10303015), KAPRIASI
Format: Final Project
Language:Indonesia
Online Access:https://digilib.itb.ac.id/gdl/view/8385
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Institution: Institut Teknologi Bandung
Language: Indonesia
id id-itb.:8385
spelling id-itb.:83852017-09-27T11:42:13Z#TITLE_ALTERNATIVE# NENG RAHAYU (NIM 10303015), KAPRIASI Indonesia Final Project INSTITUT TEKNOLOGI BANDUNG https://digilib.itb.ac.id/gdl/view/8385 Flare, solar wind, and CME (Coronal Mass Ejection) are complex Sun activities. A solar flare is a violent explosion in the Sun, resulted from the sudden release of energy stored in the magnetic fields because of the magnetic reconnection. CME are huge bubbles of gas ejected and plasma consisting primarily of protons, electrons, and ions, among those are helium, oxygen, and iron, while solar wind is a stream of charged particles. These three Sun’s activities have different effects on Earth. Study of distribution of solar wind’s high energy charged particles can help make better understanding and prediction of Sun’s activities, and the relations between one and the others, and the period.<p> <br /> <br /> <br /> ACE spacecraft is a spacecraft supported by Space Science Mission and Payload Development Division from National Aeronautics and Space Administration (NASA). A primary goal of ACE is to study and sample the composition of material from the Sun, including the corona, solar wind, interplanetary particles, the local interstellar medium/ISM, and the galaxy matter. This final project discusses the analysis of distribution of velocity and density of He+2, C+5, O+6, and Fe+10 ions from 1998 until 2006 time periode by one hour time resolution, based of data on SWICS/SWIMS instruments. Each of the four ions density distribution has a good correlation, and so does the velocity. Nevertheless, the distribution of velocity and density relate with the cycle of Sunspots. Generally, the correlation of ion distribution of density and velocity is not linear, but have a shoe pattern. The shoe pattern indicates that flare event is not always followed by the CME event, and vice versa. Flare events indicate low density and high velocity of ions, while the CME events indicate low velocity and high density of ions. Arrival time of velocity peak and density peak are different in hours or days. These were predicted so because flare and CME eject high energy particles (ions, protons, and electrons) with density and velocity in different time. Temporary, shockwave resulted from flare or CME consists of high ion velocity and high ion density. For high velocity as result by flare, the increase peak of helium density occurs before the peak of velocity. High density frontwave is in front of the velocity. Density frontwave could be classified into three frontwaves. Velocity frontwave occures after those three density frontwaves. On the contrary, in the second case, caused by domination of CME, high density frontwave occured after the velocity frontwave. text
institution Institut Teknologi Bandung
building Institut Teknologi Bandung Library
continent Asia
country Indonesia
Indonesia
content_provider Institut Teknologi Bandung
collection Digital ITB
language Indonesia
description Flare, solar wind, and CME (Coronal Mass Ejection) are complex Sun activities. A solar flare is a violent explosion in the Sun, resulted from the sudden release of energy stored in the magnetic fields because of the magnetic reconnection. CME are huge bubbles of gas ejected and plasma consisting primarily of protons, electrons, and ions, among those are helium, oxygen, and iron, while solar wind is a stream of charged particles. These three Sun’s activities have different effects on Earth. Study of distribution of solar wind’s high energy charged particles can help make better understanding and prediction of Sun’s activities, and the relations between one and the others, and the period.<p> <br /> <br /> <br /> ACE spacecraft is a spacecraft supported by Space Science Mission and Payload Development Division from National Aeronautics and Space Administration (NASA). A primary goal of ACE is to study and sample the composition of material from the Sun, including the corona, solar wind, interplanetary particles, the local interstellar medium/ISM, and the galaxy matter. This final project discusses the analysis of distribution of velocity and density of He+2, C+5, O+6, and Fe+10 ions from 1998 until 2006 time periode by one hour time resolution, based of data on SWICS/SWIMS instruments. Each of the four ions density distribution has a good correlation, and so does the velocity. Nevertheless, the distribution of velocity and density relate with the cycle of Sunspots. Generally, the correlation of ion distribution of density and velocity is not linear, but have a shoe pattern. The shoe pattern indicates that flare event is not always followed by the CME event, and vice versa. Flare events indicate low density and high velocity of ions, while the CME events indicate low velocity and high density of ions. Arrival time of velocity peak and density peak are different in hours or days. These were predicted so because flare and CME eject high energy particles (ions, protons, and electrons) with density and velocity in different time. Temporary, shockwave resulted from flare or CME consists of high ion velocity and high ion density. For high velocity as result by flare, the increase peak of helium density occurs before the peak of velocity. High density frontwave is in front of the velocity. Density frontwave could be classified into three frontwaves. Velocity frontwave occures after those three density frontwaves. On the contrary, in the second case, caused by domination of CME, high density frontwave occured after the velocity frontwave.
format Final Project
author NENG RAHAYU (NIM 10303015), KAPRIASI
spellingShingle NENG RAHAYU (NIM 10303015), KAPRIASI
#TITLE_ALTERNATIVE#
author_facet NENG RAHAYU (NIM 10303015), KAPRIASI
author_sort NENG RAHAYU (NIM 10303015), KAPRIASI
title #TITLE_ALTERNATIVE#
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url https://digilib.itb.ac.id/gdl/view/8385
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