The intermediate nebular phase of SN 2014J: onset of clumping as the source of recombination

被引：15

作者：

Mazzali, P. A. ^{[1
,2
]}

Bikmaev, I ^{[3
,4
]}

Sunyaev, R. ^{[2
]}

Ashall, C. ^{[5
]}

Prentice, S. ^{[6
]}

Tanaka, M. ^{[7
]}

Irtuganov, E. ^{[3
,4
]}

Melnikov, S. ^{[3
,4
]}

Zhuchkov, R. ^{[3
,4
]}

机构：

[1] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[2] Max Planck Inst Astrophys, Karl Schwanschild St 1, D-85748 Garching, Germany

[3] Kazan Fed Univ, Dept Astron & Satellite Geodesy, Kremlevskaya Str 18, Kazan 420008, Russia

[4] Acad Sci Republ Tatarstan, Bauman Str 20, Kazan 420111, Russia

[5] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA

[6] Trinity Coll Dublin, Dublin 2, Ireland

[7] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 494卷 / 02期

关键词：

radiative transfer; techniques: spectroscopic; supernovae: general; supernovae: individual (SN 2014J); CHANDRASEKHAR-MASS MODELS; IA SUPERNOVAE 2007ON; WHITE-DWARFS; ABUNDANCE STRATIFICATION; SPECTRAL EVOLUTION; LIGHT CURVES; 2011FE; EXPLOSION; PROGENITORS; COMPONENTS;

D O I：

10.1093/mnras/staa839

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

At the age of about 1 yr, the spectra of most Type Ia supernovae (SNe Ia) are dominated by strong forbidden nebular emission lines of Fe II and Fe III. Later observations (at about 2 yr) of the nearby SN 2011fe showed an unexpected shift of ionization to Fe I and Fell. Spectra of the very nearby SN Ia 2014J at an intermediate phase (1-1.5 yr) that are presented here show a progressive decline of Fe III emission, while Fe! is not yet strong. The decrease in ionization can be explained if the degree of clumping in the ejecta increases significantly at similar to 1.5 yr, at least in the Fe-dominated zone. Models suggest that clumps remain coherent after about one year, behaving like shrapnel. The high density in the clumps, combined with the decreasing heating rate, would then cause recombination. These data may witness the phase of transition from relatively smooth ejecta to the very clumpy morphology that is typical of SN remnants. The origin of the increased clumping may be the development of local magnetic fields.

引用

页码：2809 / 2822

页数：14

共 44 条

[31] THE PUZZLING EARLY DETECTION OF LOW VELOCITY 56Ni DECAY LINES IN SN 2014J: HINTS OF A COMPACT REMNANT
Ouyed, Rachid
Leahy, Denis
Koning, Nico
Staff, Jan
ASTROPHYSICAL JOURNAL, 2015, 801 (01):
[32] Very-high-energy gamma-ray observations of the Type Ia Supernova SN 2014J with the MAGIC telescopes
Ahnen, M.L.
Ansoldi, S.
Antonelli, L.A.
Antoranz, P.
Arcaro, C.
Babic, A.
Banerjee, B.
Bangale, P.
Barres De Almeida, U.
Barrio, J.A.
Becerra González, J.
Bednarek, W.
Bernardini, E.
Berti, A.
Biasuzzi, B.
Biland, A.
Blanch, O.
Bonnefoy, S.
Bonnoli, G.
Borracci, F.
Bretz, T.
Carosi, R.
Carosi, A.
Chatterjee, A.
Colin, P.
Colombo, E.
Contreras, J.L.
Cortina, J.
Covino, S.
Cumani, P.
Da Vela, P.
Dazzi, F.
De Angelis, A.
De Lotto, B.
De Onã Wilhelmi, E.
DI Pierro, F.
Doert, M.
Domínguez, A.
Dominis Prester, D.
Dorner, D.
Doro, M.
Einecke, S.
Eisenacher Glawion, D.
Elsaesser, D.
Engelkemeier, M.
Fallah Ramazani, V.
Fernández-Barral, A.
Fidalgo, D.
Fonseca, M.V.
Font, L.
Astronomy and Astrophysics, 2017, 602
[33] Very-high-energy Gamma-ray Observations Of The Type Ia Supernova SN 2014J With The MAGIC Telescopes
Fernandez-Barral, A.
Fruck, C.
Blanchi, O.
de Ona Wilhelmi, E.
HIGH ENERGY GAMMA-RAY ASTRONOMY, 2017, 1792
[34] Very-high-energy gamma-ray observations of the Type Ia Supernova SN 2014J with the MAGIC telescopes
Ahnen, M. L.
Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Arcaro, C.
Babic, A.
Banerjee, B.
Bangale, P.
de Almeida, U. Barres
Barrio, J. A.
Becerra Gonzalez, J.
Bednarek, W.
Bernardini, E.
Berti, A.
Biasuzzi, B.
Biland, A.
Blanch, O.
Bonnefoy, S.
Bonnoli, G.
Borracci, F.
Bretz, T.
Carosi, R.
Carosi, A.
Chatterjee, A.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Covino, S.
Cumani, P.
Da Vela, P.
Dazzi, F.
De Angelis, A.
De Lotto, B.
de Ona Wilhelmi, E.
Di Pierro, F.
Doert, M.
Dominguez, A.
Prester, D. Dominis
Dorner, D.
Doro, M.
Einecke, S.
Glawion, D. Eisenacher
Elsaesser, D.
Engelkemeier, M.
Ramazani, V. Fallah
Fernandez-Barral, A.
Fidalgo, D.
Fonseca, M. V.
Font, L.
ASTRONOMY & ASTROPHYSICS, 2017, 602
[35] Progenitor constraints on the Type Ia supernova SN 2014J from Hubble Space Telescope H β and [O III] observations
Graur, Or
Woods, Tyrone E.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2019, 484 (01) : L79 - L84
[36] Photometric and spectroscopic observations, and abundance tomography modelling of the Type Ia supernova SN 2014J located in M82
Ashall, C.
Mazzali, P.
Bersier, D.
Hachinger, S.
Phillips, M.
Percival, S.
James, P.
Maguire, K.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2014, 445 (04) : 4424 - 4434
[37] MID-IR SPECTRA OF TYPE Ia SN 2014J IN M82 SPANNING THE FIRST 4 MONTHS
Telesco, Charles M.
Hoeflich, Peter
Li, Dan
Alvarez, Carlos
Wright, Christopher M.
Barnes, Peter J.
Fernandez, Sergio
Hough, James H.
Levenson, N. A.
Marinas, Naibi
Packham, Christopher
Pantin, Eric
Rebolo, Rafael
Roche, Patrick
Zhang, Han
ASTROPHYSICAL JOURNAL, 2015, 798 (02):
[38] Late-time Observations of the Type Ia Supernova SN 2014J with the Hubble Space Telescope Wide Field Camera 3
Graur, Or
ASTROPHYSICAL JOURNAL, 2019, 870 (01):
[39] DIFFUSE INTERSTELLAR BANDS VERSUS KNOWN ATOMIC AND MOLECULAR SPECIES IN THE INTERSTELLAR MEDIUM OF M82 TOWARD SN 2014J
Welty, Daniel E.
Ritchey, Adam M.
Dahlstrom, Julie A.
York, Donald G.
ASTROPHYSICAL JOURNAL, 2014, 792 (02):
[40] Late-time Flattening of Type Ia Supernova Light Curves: Constraints from SN 2014J in M82
Yang, Yi
Wang, Lifan
Baade, Dietrich
Brown, Peter. J.
Cikota, Aleksandar
Cracraft, Misty
Hoflich, Peter A.
Maund, Justyn R.
Patat, Ferdinando
Sparks, William B.
Spyromilio, Jason
Stevance, Heloise F.
Wang, Xiaofeng
Wheeler, J. Craig
ASTROPHYSICAL JOURNAL, 2018, 852 (02):

← 1 2 3 4 5 →