Spectral Mixture Modeling with Laboratory Near-Infrared Data I: Insights into Compositional Analysis of Europa
Fuente:
arXiv
Salvato in:
| Autore principale: | |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2025
|
| Soggetti: | |
| Accesso online: | |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866914094881177600 |
|---|---|
| author | Emran, A. |
| author_facet | Emran, A. |
| contents | Europa's surface composition and physical characteristics are commonly constrained using spectral deconvolution through linear mixture (LM) modeling and radiative transfer-based (RT) intimate mixture modeling. Here, I compared the results of these two spectral modeling- LM versus RT- against laboratory spectra of water (H$_{2}$O) ice and sulfuric acid octahydrate (SAO; H$_{2}$SO$_{4}$$\cdot$8H$_{2}$O) mixtures measured at near-infrared wavelengths ($\sim$1.2-2.5 $μ$m) with grain sizes of 90-106 $μ$m (Hayes and Li, 2025). The modeled abundances indicate that the RT more closely reproduces the laboratory abundances, with deviations within $\pm$5% for both H$_{2}$O ice and H$_{2}$SO$_{4}$$\cdot$8H$_{2}$O with $\sim$100 $μ$m grains. In contrast, the LM shows slightly larger discrepancies, typically ranging from $\pm$5-15% from the true abundances. Interestingly, both LM and RT tend to consistently overestimate the abundance of H$_{2}$SO$_{4}$$\cdot$8H$_{2}$O and underestimate H$_{2}$O ice across all mixtures. Nonetheless, when H$_{2}$SO$_{4}$$\cdot$8H$_{2}$O either dominates (>80% as observed on Europa's trailing hemisphere; Carlson et al. 2005) or is present only in trace amounts ($\sim$10% on areas in Europa's leading hemisphere; Dalton III et al. 2013; Ligier et al. 2016), both the LM and RT render acceptable results within $\pm$10% uncertainty. Thus, spectral modeling using the RT is preferred for constraining the surface composition across Europa, although the LM remains viable in specific compositional regimes. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_03436 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Spectral Mixture Modeling with Laboratory Near-Infrared Data I: Insights into Compositional Analysis of Europa Emran, A. Earth and Planetary Astrophysics Instrumentation and Methods for Astrophysics Europa's surface composition and physical characteristics are commonly constrained using spectral deconvolution through linear mixture (LM) modeling and radiative transfer-based (RT) intimate mixture modeling. Here, I compared the results of these two spectral modeling- LM versus RT- against laboratory spectra of water (H$_{2}$O) ice and sulfuric acid octahydrate (SAO; H$_{2}$SO$_{4}$$\cdot$8H$_{2}$O) mixtures measured at near-infrared wavelengths ($\sim$1.2-2.5 $μ$m) with grain sizes of 90-106 $μ$m (Hayes and Li, 2025). The modeled abundances indicate that the RT more closely reproduces the laboratory abundances, with deviations within $\pm$5% for both H$_{2}$O ice and H$_{2}$SO$_{4}$$\cdot$8H$_{2}$O with $\sim$100 $μ$m grains. In contrast, the LM shows slightly larger discrepancies, typically ranging from $\pm$5-15% from the true abundances. Interestingly, both LM and RT tend to consistently overestimate the abundance of H$_{2}$SO$_{4}$$\cdot$8H$_{2}$O and underestimate H$_{2}$O ice across all mixtures. Nonetheless, when H$_{2}$SO$_{4}$$\cdot$8H$_{2}$O either dominates (>80% as observed on Europa's trailing hemisphere; Carlson et al. 2005) or is present only in trace amounts ($\sim$10% on areas in Europa's leading hemisphere; Dalton III et al. 2013; Ligier et al. 2016), both the LM and RT render acceptable results within $\pm$10% uncertainty. Thus, spectral modeling using the RT is preferred for constraining the surface composition across Europa, although the LM remains viable in specific compositional regimes. |
| title | Spectral Mixture Modeling with Laboratory Near-Infrared Data I: Insights into Compositional Analysis of Europa |
| topic | Earth and Planetary Astrophysics Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2510.03436 |