Summary of the pros and cons of each of the progenitor systems considered for AT2018kzr.
. | Ultrastripped . | Accretion-induced . | Double WD . | Merger of a WD . |
---|---|---|---|---|
. | core-collapse SN . | collapse of an ONe WD . | merger systems . | with an NS/BH . |
Peak brightness | Bad | Possiblea | Good | Possibleb |
Light-curve evolution | Bad | Possiblec | Good | Good |
Velocity of ejecta | Good | Bad | Good | Goodd |
Ejecta mass | Good | Good | Good | Possiblee |
Bulk composition | Good | Bad | Bad | Good |
Fe/Ni ratio | Bad | Bad | Bad | Good |
. | Ultrastripped . | Accretion-induced . | Double WD . | Merger of a WD . |
---|---|---|---|---|
. | core-collapse SN . | collapse of an ONe WD . | merger systems . | with an NS/BH . |
Peak brightness | Bad | Possiblea | Good | Possibleb |
Light-curve evolution | Bad | Possiblec | Good | Good |
Velocity of ejecta | Good | Bad | Good | Goodd |
Ejecta mass | Good | Good | Good | Possiblee |
Bulk composition | Good | Bad | Bad | Good |
Fe/Ni ratio | Bad | Bad | Bad | Good |
aCapable of producing a magnetar, which can power the light curve.
bCapable of reaching the observed luminosity of AT2018kzr, with the help of high-velocity winds launched off the disc.
cLight-curve evolution too fast in the models discussed, but a higher ejecta mass would act to extend the light curve.
dThe bulk velocity of the ejecta material agrees with our photospheric estimates for ejecta velocity.
eThe ejecta mass obtained from light-curve modelling is lower than that estimated from the models discussed, but these values are dependent on the specific merger, which make it difficult to get good approximations.
Summary of the pros and cons of each of the progenitor systems considered for AT2018kzr.
. | Ultrastripped . | Accretion-induced . | Double WD . | Merger of a WD . |
---|---|---|---|---|
. | core-collapse SN . | collapse of an ONe WD . | merger systems . | with an NS/BH . |
Peak brightness | Bad | Possiblea | Good | Possibleb |
Light-curve evolution | Bad | Possiblec | Good | Good |
Velocity of ejecta | Good | Bad | Good | Goodd |
Ejecta mass | Good | Good | Good | Possiblee |
Bulk composition | Good | Bad | Bad | Good |
Fe/Ni ratio | Bad | Bad | Bad | Good |
. | Ultrastripped . | Accretion-induced . | Double WD . | Merger of a WD . |
---|---|---|---|---|
. | core-collapse SN . | collapse of an ONe WD . | merger systems . | with an NS/BH . |
Peak brightness | Bad | Possiblea | Good | Possibleb |
Light-curve evolution | Bad | Possiblec | Good | Good |
Velocity of ejecta | Good | Bad | Good | Goodd |
Ejecta mass | Good | Good | Good | Possiblee |
Bulk composition | Good | Bad | Bad | Good |
Fe/Ni ratio | Bad | Bad | Bad | Good |
aCapable of producing a magnetar, which can power the light curve.
bCapable of reaching the observed luminosity of AT2018kzr, with the help of high-velocity winds launched off the disc.
cLight-curve evolution too fast in the models discussed, but a higher ejecta mass would act to extend the light curve.
dThe bulk velocity of the ejecta material agrees with our photospheric estimates for ejecta velocity.
eThe ejecta mass obtained from light-curve modelling is lower than that estimated from the models discussed, but these values are dependent on the specific merger, which make it difficult to get good approximations.
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