The Phillips relation of 'Normal' type Ia Supernovae
The use of Type Ia Supernovae (SNe Ia) as distance indicators relies on the calibration of their brightness using the observed property that brighter SNe have broader, slower light curves. Among possible causes are different masses of the progenitor white dwarfs or different opacities. We construct...
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| Format: | Conference item |
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2001
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| _version_ | 1797072110254817280 |
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| author | Mazzali, P |
| author_facet | Mazzali, P |
| author_sort | Mazzali, P |
| collection | OXFORD |
| description | The use of Type Ia Supernovae (SNe Ia) as distance indicators relies on the calibration of their brightness using the observed property that brighter SNe have broader, slower light curves. Among possible causes are different masses of the progenitor white dwarfs or different opacities. We construct Chandrasekhar-mass models which synthesize different amounts of Ni-56, and compute their bolometric light curves and spectra. Since opacity in SNe Ia at early times is due mostly to spectral lines, and Fe-peak ions have many more lines than lighter ions, the opacity depends on the synthesized Ni-56 mass and on the temperature in the ejecta. Bolometric light curves computed using these prescriptions reproduce the relation between brightness and decline rate. The synthetic spectra compare well with spectra of spectroscopically normal SNe Ia which cover a similar Deltam(15)(B) range. The change in colour of the spectra between maximum and two weeks later allows the observed relation between M-B(Max) and Deltam(15)(B) to be reproduced. |
| first_indexed | 2024-03-06T23:02:55Z |
| format | Conference item |
| id | oxford-uuid:62cb84d3-e4c3-4027-8c99-3fb530a664da |
| institution | University of Oxford |
| last_indexed | 2024-03-06T23:02:55Z |
| publishDate | 2001 |
| record_format | dspace |
| spelling | oxford-uuid:62cb84d3-e4c3-4027-8c99-3fb530a664da2022-03-26T18:08:32ZThe Phillips relation of 'Normal' type Ia SupernovaeConference itemhttp://purl.org/coar/resource_type/c_5794uuid:62cb84d3-e4c3-4027-8c99-3fb530a664daSymplectic Elements at Oxford2001Mazzali, PThe use of Type Ia Supernovae (SNe Ia) as distance indicators relies on the calibration of their brightness using the observed property that brighter SNe have broader, slower light curves. Among possible causes are different masses of the progenitor white dwarfs or different opacities. We construct Chandrasekhar-mass models which synthesize different amounts of Ni-56, and compute their bolometric light curves and spectra. Since opacity in SNe Ia at early times is due mostly to spectral lines, and Fe-peak ions have many more lines than lighter ions, the opacity depends on the synthesized Ni-56 mass and on the temperature in the ejecta. Bolometric light curves computed using these prescriptions reproduce the relation between brightness and decline rate. The synthetic spectra compare well with spectra of spectroscopically normal SNe Ia which cover a similar Deltam(15)(B) range. The change in colour of the spectra between maximum and two weeks later allows the observed relation between M-B(Max) and Deltam(15)(B) to be reproduced. |
| spellingShingle | Mazzali, P The Phillips relation of 'Normal' type Ia Supernovae |
| title | The Phillips relation of 'Normal' type Ia Supernovae |
| title_full | The Phillips relation of 'Normal' type Ia Supernovae |
| title_fullStr | The Phillips relation of 'Normal' type Ia Supernovae |
| title_full_unstemmed | The Phillips relation of 'Normal' type Ia Supernovae |
| title_short | The Phillips relation of 'Normal' type Ia Supernovae |
| title_sort | phillips relation of normal type ia supernovae |
| work_keys_str_mv | AT mazzalip thephillipsrelationofnormaltypeiasupernovae AT mazzalip phillipsrelationofnormaltypeiasupernovae |