ALMA observations of Molecules in Supernova 1987A
Supernova (SN) 1987A has provided a unique opportunity to study how SN ejecta evolve in 30 years time scale. We report our ALMA spectral observations of SN 1987A, taken in 2014, 2015 and 2016, with detections of CO, 28SiO, HCO+ and SO, with weaker lines of 29SiO. We find a dip in the SiO line profi...
| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Format: | Journal article |
| Published: |
Cambridge University Press
2017
|
| _version_ | 1826296180789739520 |
|---|---|
| author | Matsuura, M Indebetouw, R Woosley, S Bujarrabal, V Abellán, F McCray, R Kamenetzky, J Fransson, C Barlow, M Gomez, H Cigan, P De Looze, I Spyromilio, J Staveley-Smith, L Zanardo, G Roche, P Larsson, J Viti, S van Loon, J Wheeler, J Baes, M Chevalier, R Lundqvist, P Marcaide, J Dwek, E Meixner, M Ng, C Sonneborn, G Yates, J |
| author_facet | Matsuura, M Indebetouw, R Woosley, S Bujarrabal, V Abellán, F McCray, R Kamenetzky, J Fransson, C Barlow, M Gomez, H Cigan, P De Looze, I Spyromilio, J Staveley-Smith, L Zanardo, G Roche, P Larsson, J Viti, S van Loon, J Wheeler, J Baes, M Chevalier, R Lundqvist, P Marcaide, J Dwek, E Meixner, M Ng, C Sonneborn, G Yates, J |
| author_sort | Matsuura, M |
| collection | OXFORD |
| description | Supernova (SN) 1987A has provided a unique opportunity to study how SN ejecta evolve in 30 years time scale. We report our ALMA spectral observations of SN 1987A, taken in 2014, 2015 and 2016, with detections of CO, 28SiO, HCO+ and SO, with weaker lines of 29SiO. We find a dip in the SiO line profiles, suggesting that the ejecta morphology is likely elongated. The difference of the CO and SiO line profiles is consistent with hydrodynamic simulations, which show that Rayleigh-Taylor instabilities causes mixing of gas, with heavier elements much more disturbed, making more elongated structure. Using 28SiO and its isotopologues, Si isotope ratios were estimated for the first time in SN 1987A. The estimated ratios appear to be consistent with theoretical predictions of inefficient formation of neutron rich atoms at lower metallicity, such as observed in the Large Magellanic Cloud (about half a solar metallicity). The deduced large HCO+ mass and small SiS mass, which are inconsistent to the predictions of chemical model, might be explained by some mixing of elements immediately after the explosion. The mixing might have made some hydrogen from the envelope to sink into carbon and oxygen-rich zone during early days after the explosion, enabling the formation of a substantial mass of HCO+. Oxygen atoms may penetrate into silicon and sulphur zone, suppressing formation of SiS. Our ALMA observations open up a new window to investigate chemistry, dynamics and explosive-nucleosynthesis in supernovae. |
| first_indexed | 2024-03-07T04:12:22Z |
| format | Journal article |
| id | oxford-uuid:c845e5bb-358f-4f21-a80c-8bb1db968053 |
| institution | University of Oxford |
| last_indexed | 2024-03-07T04:12:22Z |
| publishDate | 2017 |
| publisher | Cambridge University Press |
| record_format | dspace |
| spelling | oxford-uuid:c845e5bb-358f-4f21-a80c-8bb1db9680532022-03-27T06:51:02ZALMA observations of Molecules in Supernova 1987AJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:c845e5bb-358f-4f21-a80c-8bb1db968053Symplectic Elements at OxfordCambridge University Press2017Matsuura, MIndebetouw, RWoosley, SBujarrabal, VAbellán, FMcCray, RKamenetzky, JFransson, CBarlow, MGomez, HCigan, PDe Looze, ISpyromilio, JStaveley-Smith, LZanardo, GRoche, PLarsson, JViti, Svan Loon, JWheeler, JBaes, MChevalier, RLundqvist, PMarcaide, JDwek, EMeixner, MNg, CSonneborn, GYates, JSupernova (SN) 1987A has provided a unique opportunity to study how SN ejecta evolve in 30 years time scale. We report our ALMA spectral observations of SN 1987A, taken in 2014, 2015 and 2016, with detections of CO, 28SiO, HCO+ and SO, with weaker lines of 29SiO. We find a dip in the SiO line profiles, suggesting that the ejecta morphology is likely elongated. The difference of the CO and SiO line profiles is consistent with hydrodynamic simulations, which show that Rayleigh-Taylor instabilities causes mixing of gas, with heavier elements much more disturbed, making more elongated structure. Using 28SiO and its isotopologues, Si isotope ratios were estimated for the first time in SN 1987A. The estimated ratios appear to be consistent with theoretical predictions of inefficient formation of neutron rich atoms at lower metallicity, such as observed in the Large Magellanic Cloud (about half a solar metallicity). The deduced large HCO+ mass and small SiS mass, which are inconsistent to the predictions of chemical model, might be explained by some mixing of elements immediately after the explosion. The mixing might have made some hydrogen from the envelope to sink into carbon and oxygen-rich zone during early days after the explosion, enabling the formation of a substantial mass of HCO+. Oxygen atoms may penetrate into silicon and sulphur zone, suppressing formation of SiS. Our ALMA observations open up a new window to investigate chemistry, dynamics and explosive-nucleosynthesis in supernovae. |
| spellingShingle | Matsuura, M Indebetouw, R Woosley, S Bujarrabal, V Abellán, F McCray, R Kamenetzky, J Fransson, C Barlow, M Gomez, H Cigan, P De Looze, I Spyromilio, J Staveley-Smith, L Zanardo, G Roche, P Larsson, J Viti, S van Loon, J Wheeler, J Baes, M Chevalier, R Lundqvist, P Marcaide, J Dwek, E Meixner, M Ng, C Sonneborn, G Yates, J ALMA observations of Molecules in Supernova 1987A |
| title | ALMA observations of Molecules in Supernova 1987A |
| title_full | ALMA observations of Molecules in Supernova 1987A |
| title_fullStr | ALMA observations of Molecules in Supernova 1987A |
| title_full_unstemmed | ALMA observations of Molecules in Supernova 1987A |
| title_short | ALMA observations of Molecules in Supernova 1987A |
| title_sort | alma observations of molecules in supernova 1987a |
| work_keys_str_mv | AT matsuuram almaobservationsofmoleculesinsupernova1987a AT indebetouwr almaobservationsofmoleculesinsupernova1987a AT woosleys almaobservationsofmoleculesinsupernova1987a AT bujarrabalv almaobservationsofmoleculesinsupernova1987a AT abellanf almaobservationsofmoleculesinsupernova1987a AT mccrayr almaobservationsofmoleculesinsupernova1987a AT kamenetzkyj almaobservationsofmoleculesinsupernova1987a AT franssonc almaobservationsofmoleculesinsupernova1987a AT barlowm almaobservationsofmoleculesinsupernova1987a AT gomezh almaobservationsofmoleculesinsupernova1987a AT ciganp almaobservationsofmoleculesinsupernova1987a AT deloozei almaobservationsofmoleculesinsupernova1987a AT spyromilioj almaobservationsofmoleculesinsupernova1987a AT staveleysmithl almaobservationsofmoleculesinsupernova1987a AT zanardog almaobservationsofmoleculesinsupernova1987a AT rochep almaobservationsofmoleculesinsupernova1987a AT larssonj almaobservationsofmoleculesinsupernova1987a AT vitis almaobservationsofmoleculesinsupernova1987a AT vanloonj almaobservationsofmoleculesinsupernova1987a AT wheelerj almaobservationsofmoleculesinsupernova1987a AT baesm almaobservationsofmoleculesinsupernova1987a AT chevalierr almaobservationsofmoleculesinsupernova1987a AT lundqvistp almaobservationsofmoleculesinsupernova1987a AT marcaidej almaobservationsofmoleculesinsupernova1987a AT dweke almaobservationsofmoleculesinsupernova1987a AT meixnerm almaobservationsofmoleculesinsupernova1987a AT ngc almaobservationsofmoleculesinsupernova1987a AT sonneborng almaobservationsofmoleculesinsupernova1987a AT yatesj almaobservationsofmoleculesinsupernova1987a |