Table 1
Typical properties of different flaring source categories.
| Category | Γ | t var | L bol | E p,max | E ν,max | ϵth [ϵb] | ηp Φγ,min | DL,max [ zmax ] | |
| (s) | (erg s-1) | (PeV) | (PeV) | (eV) | (ph cm-2 s-1) | ||||
|
|
|||||||||
| HL GRBs | 300 | 10-3−1 | 1049−53 | 104−6 | 0.1−103 | 1−103 | 104−8 | [ 3 ] | |
|
|
|||||||||
| HL GRBs | 100 | 10-3−1 | 1049−53 | 103−5 | 10-3−10 | 10−103 | 101−4 | [ 3.2 ] | |
| Blazar flares | 102−106 | 1044−48 | 102−4 | 10−103 | 102−104 | 107−11 | [ 3 × 10-4 ] | ||
| BH mergers | 104−106.7 | 1043−46 | 102−3 | 1−102 | 103−104 | 109−12 | − | ||
| NS mergers | 103−104 | 1046−48 | 103−4 | 102−103 | 102−103 | 107−9 | − | ||
| WD mergers | 102−104 | 1044−46 | 102−3 | 1−102 | 103−104 | 109−11 | − | ||
|
|
|||||||||
| Blazar flares | 10 | 102−106 | 1044−48 | 103−5 | 10−104 | 0.1−10 | 103−7 | [ 0.7 ] | |
| LL GRBs | 10−103 | 1046−48 | 104−5 | 1−103 | 0.1−1 | 103−5 | 10 Mpc | ||
| Magnetar GF | 10-3−0.1 | 1044−47 | 102−3 | 10-4−0.1 | [ 105 ] | 104−7 | 0.4 Mpc | ||
| TDEs | 102−104 | 1043−48 | 103−5 | 10−103 | [ 104 ] | 103−8 | 20 Mpc | ||
| BH mergers | 104−106.7 | 1043−46 | 103−4 | 10−103 | 1−10 | 105−8 | − | ||
| NS mergers | 103−104 | 1046−48 | 104−5 | 102−103 | 10-1−1 | 103−5 | − | ||
| WD mergers | 102−104 | 1044−46 | 103−4 | 102−103 | 1−10 | 105−7 | − | ||
|
|
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| SLSNe | 1 | 105−107 | 1043−45 | 104−5 | 10−103 | 10-3−10-2 | 102−4 | 4 Mpc | |
| SNe | 105−107 | 1040−43 | 102−4 | 10−103 | 10-2−1 | 103−7 | 40 kpc | ||
| Novae | 105−107 | 1038−40 | 101−2 | 1−10 | 1−10 | 107−9 | 40 pc | ||
| Magnetar IB | 1−40 | 1041−43 | 103 | 0.1−1 | 0.1−1 | 104−6 | 200 pc | ||
| Magnetar SB | 0.1−1 | 1039−41 | 102 | 10-2 | 0.1 | 106−8 | 2 pc | ||
| BH mergers | 104−106.7 | 1043−46 | 103−5 | 1−102 | 10-3−10-2 | 101−4 | − | ||
| NS mergers | 103−104 | 1046−48 | 102−3 | 10-2−1 | 10-2−10-1 | 10− 1−1 | − | ||
| WD mergers | 102−104 | 1044−46 | 102−4 | 10-2−10 | 10-2−10-1 | 101−3 | − | ||
Notes. We recall the ranges of values for the bulk Lorentz factor Γ, time variability tvar, and apparent bolometric luminosity Lbol for each category and the derived maximum energy of protons Ep,max, maximum energy of neutrinos Eν,max, threshold energy ϵth (for soft photon spectra), and the required flux for detectability Φγ,min. The flux can be converted from ph cm-2 s-1 into Jy by multiplying by ~ 10-3. DL,max or zmax are the order of magnitude of the maximum distance or redshift at which we can expect to detect an associated neutrino flare with IceCube. Here ηB = ηp = 1, but the most conservative estimate should use ηp = 100. Starred types of sources should be viewed with care because of possible hidden radiation (Sect. 6.2).
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