Table 2
Overview of selected X-ray instruments and the resulting power-law indices.
| Power-law(c) | m for: LX ∝ Φm(d) | ||||
|---|---|---|---|---|---|
| Energy range(b) | index α for: | Nanoflares | Alfvén waves | ||
| Instrument | Detector/Filter(a) | [keV] | R ∝ Tα | (β = 2) | (β = 1) |
| XMM/EPIC | pn_med | 0.05–12 | 0.7 ± 0.03 | 1.0 ± 0.3 | 0.8 ± 0.2 |
| Einstein | ipc | 0.1–5 | 0.7 ± 0.04 | 1.0 ± 0.3 | 0.8 ± 0.2 |
| Chandra/LETG | acis-s_order0 | 0.07–10 | 1.2 ± 0.1 | 1.1 ± 0.3 | 0.9 ± 0.2 |
| ROSAT | pspc_brn | 0.1–2.3 | 1.6 ± 0.1 | 1.2 ± 0.3 | 0.9 ± 0.2 |
| XMM/RGS | rgs2_o1 | 0.3–2.5 | 1.8 ± 0.2 | 1.3 ± 0.3 | 1.0 ± 0.3 |
| Hinode/XRT | Al-poly | 0.2–3 | 2.1 ± 0.2 | 1.3 ± 0.4 | 1.0 ± 0.3 |
| Chandra/HETG | acis-s_heg1meg1 | 0.4–10 | 3.1 ± 0.3 | 1.6 ± 0.4 | 1.2 ± 0.3 |
Notes. (a) The detector or filter type refers to the naming convention as used in the CHIANTI database for the effective area for the respective instrument-detector-filter combination. (b)The energy ranges are estimates based on the effective areas as listed in CHIANTI or as available in SOLARSOFT (in the case of Hinode/XRT). (c) The power-law fits to the temperatureresponses R(T) as shown in Fig. 1 have been performed in the range of log10 T [K] from 5.9 to 6.9 (for ROSAT the lower end of the fit range is 6.2 to avoid the bump at lower temperatures). (d) The power-law indices m as defined in Eq. (13), are calculated for γ = 1 as in Eq. (5) and δ = 0.819 as in Eq. (7) for the two heating processes (nanoflares, Alfvén waves; see Sect. 3).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.