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<p>In this paper, we study the wave travel-time shift signature of two distinct magnetic models of sunspots, namely a monolithic model of varying sizes and a cluster (or spaghetti) model of different configurations (compact and loose) and sizes. To this end, we use numerical simulations to propagate an <InlineEquation ID="IEq1"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="11207_2025_2436_Article_IEq1.gif" Format="GIF" Height="17" Rendition="HTML" Resolution="72" Type="Linedraw" Width="14" /> </InlineMediaObject> <EquationSource Format="MATHML"><math> <mi>f</mi> </math></EquationSource> <EquationSource Format="TEX">$f$</EquationSource> </InlineEquation>-mode wave packet through these magnetic structures. We have shown that the region <InlineEquation ID="IEq2"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="11207_2025_2436_Article_IEq2.gif" Format="GIF" Height="16" Rendition="HTML" Resolution="72" Type="Linedraw" Width="41" /> </InlineMediaObject> <EquationSource Format="MATHML"><math> <mi>y</mi> <mo>=</mo> <mn>0</mn> </math></EquationSource> <EquationSource Format="TEX">$y=0$</EquationSource> </InlineEquation> behind the sunspot can be contaminated by caustics that emerge from both models, making the interpretation of the travel-time ambiguous. However, the location and characteristics (amplitude and pattern) of these caustics can be used as observational indicators to distinguish between a monolithic and a clustered model, as well as to differentiate between a compact and an open cluster configuration. These results are a contribution to probe the subsurface structure of sunspots and plages in the context of time-distance helioseismology.</p>

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Travel Time Estimation from Numerical Simulations of f-Mode Propagation Through Sunspot Models and Plages

  • 期刊论文

  • 发表日期：

    2025年2月12日

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  • Khalil Daiffallah,
  • Omar Boumia

摘要

In this paper, we study the wave travel-time shift signature of two distinct magnetic models of sunspots, namely a monolithic model of varying sizes and a cluster (or spaghetti) model of different configurations (compact and loose) and sizes. To this end, we use numerical simulations to propagate an f $f$ -mode wave packet through these magnetic structures. We have shown that the region y = 0 $y=0$ behind the sunspot can be contaminated by caustics that emerge from both models, making the interpretation of the travel-time ambiguous. However, the location and characteristics (amplitude and pattern) of these caustics can be used as observational indicators to distinguish between a monolithic and a clustered model, as well as to differentiate between a compact and an open cluster configuration. These results are a contribution to probe the subsurface structure of sunspots and plages in the context of time-distance helioseismology.