Table 5
Detection limit of LOFAR LBA beam-formed observations found by observing “Jupiter as an exoplanet”.
| SJ (ref; Jy at 5 AU) | Distance (pc) | Stokes-I αJ | Stokes-V αJ | |
|---|---|---|---|---|
| 4 × 104(a) | 5 | 1 × 107 | 1 × 106 | |
| ” | 10 | 4 × 107 | 4 × 106 | |
| ” | 20 | 2 × 108 | 2 × 107 | |
| 4 × 105(b) | 5 | 1 × 106 | 1 × 105 | |
| ” | 10 | 4 × 106 | 4 × 105 | |
| ” | 20 | 2 × 107 | 2 × 106 | |
| 6 × 106(c) | 5 | 6 × 104 | 6 × 103 | |
| ” | 10 | 3 × 105 | 3 × 104 | |
| ” | 20 | 1 × 106 | 1 × 105 | |
Notes. All calculations were done with Eq. (21) where the scaling factor α = 10−3.5 for Stokes-I and α = 10−4.5 for Stokes-V and SJ (obs) = 3 × 104 Jy (Sect. 3.1, Fig. 2). (a) The level of Jupiter’s burst emission exceeded in ≥50% of Jupiter bursts (Zarka et al. 2004, Fig. 7). (b)The mean level of Jupiter’s burst emission exceeded in ~1% of Jupiter bursts. (c)Maximum peak of Jupiter’s S-burst emission (Queinnec & Zarka 2001).
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