| DC 欄位 |
值 |
語言 |
| DC.contributor | 太空科學與工程學系 | zh_TW |
| DC.creator | 蒙馬林 | zh_TW |
| DC.creator | Merlin Malonzo Mendoza | en_US |
| dc.date.accessioned | 2024-7-29T07:39:07Z | |
| dc.date.available | 2024-7-29T07:39:07Z | |
| dc.date.issued | 2024 | |
| dc.identifier.uri | http://ir.lib.ncu.edu.tw:444/thesis/view_etd.asp?URN=109623602 | |
| dc.contributor.department | 太空科學與工程學系 | zh_TW |
| DC.description | 國立中央大學 | zh_TW |
| DC.description | National Central University | en_US |
| dc.description.abstract | 太陽小黑斑是光球層中的小黑點，是具有集中的磁通量但沒有半影的小黑點。它們經常被觀察到在其整個生命週期中會展現水平運動。我們從 Spaceweather HMI Active Region Patches (SHARP)在 2011 年至 2018 年間的影像找到 61 個緊湊型太陽小黑斑，研究它們的水平運動與其可觀察到的物理量之間是否存在任何關係。我們的結果顯示，小黑斑運動的方向(ϕt)和最大正磁壓差的方向 (ϕdPo)通常是平行或反平行的、平行的情況比反平行的情況多。我們的分析也顯示，移動小黑斑前端的磁場比後方的磁場更傾斜，水平和徑向磁場比後方的更強。，而且小黑斑在外層（內層）的前（後）方平均較亮。研究19 對雙極性小黑斑的研究顯示，ϕdPo 在北（南）半球略微指向北（南）。同ㄧ對的前導和後導小黑斑的⟨∆Pmag⟩的符號總是相反，我們稱之為 ∆Pmag 規則。最後平行和反平行情況的相關係數都高於 0.74。儘管相關性很高，使用轉移熵（transfer entropy）進行的因果關係分析顯示，ϕt 與 ϕdPo 之間沒有因果關係。 | zh_TW |
| dc.description.abstract | Solar pores are small dark spots in the photosphere with concen-
trated magnetic flux and without a penumbra. They are often observed
to exhibit horizontal motions throughout their lifetime. We examine 61
compact solar pores identified from the Spaceweather HMI Active Re-
gion Patches (SHARP) from 2011 to 2018 to investigate whether any
relationships may exist between the pore movement and its observable
physical quantities. Our results show that the direction of movement
(ϕt) and the direction of maximum positive magnetic pressure differ-
ence (ϕdPo) of the solar pores are often either parallel or anti-parallel,
with more parallel cases than the anti-parallel cases. Our analysis also
indicates that the magnetic fields at the front side of the moving pores
are more likely to be more inclined with stronger horizontal and radial
fields than those at the back side, and that the pores are on average
brighter at the front (back) sides of their outer (inner) layer. An exam-
ination of 19 pairs of bipolar pores reveal that ϕdPo is slightly pointing
towards the north (south) in the northern (southern) hemisphere, and
the signs of ⟨∆Pmag⟩ for the leading and trailing pores of the pair are
always opposite, which we call the ∆Pmag rule. Finally, the correlation
coefficients between ϕt and ϕdPo are both higher than 0.74 for the par-
allel and anti-parallel cases. Despite the high correlation, the causality
analysis using transfer entropy reveal no causal relationships between ϕt
and ϕdPo | en_US |
| DC.subject | solar physics | zh_TW |
| DC.subject | solar pores | zh_TW |
| DC.subject | solar magnetic fields | zh_TW |
| DC.subject | solar magnetic flux emergence | zh_TW |
| DC.subject | transfer entropy | zh_TW |
| DC.subject | causality analysis | zh_TW |
| DC.subject | Solar physics | en_US |
| DC.subject | solar pores | en_US |
| DC.subject | solar magnetic fields | en_US |
| DC.subject | solar magnetic flux emergence | en_US |
| DC.subject | transfer entropy | en_US |
| DC.subject | causality analysis | en_US |
| DC.title | On the Motion of Solar Pores and its Manifestations on Observable Physical Quantities at the Photosphere | en_US |
| dc.language.iso | en_US | en_US |
| DC.type | 博碩士論文 | zh_TW |
| DC.type | thesis | en_US |
| DC.publisher | National Central University | en_US |