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The Transitional Type Ibn/IIn SN 2022pda, with Pre-explosion Outbursts and a Double-peaked Light Curve

  • Authors: Y.-Z. Cai, 永志 蔡, A. Pastorello, R. Chiba, T. J. Moriya, A. Reguitti, L. Tartaglia, S. Moran, S. Campana, Z.-Y. Wang, J.-W. Zhao, J. P. Anderson, S. Benetti, S. J. Brennan, E. Cappellaro, K. C. Chambers, T.-W. Chen, Z.-H. Chen, T. de Boer, Y.-Z. Dong, J. Duarte, N. Elias-Rosa, M. Fraser, W.-P. Gan, H. Gao, M. Gromadzki, G. Hosseinzadeh, D. A. Howell, C. Inserra, T. Kangas, E. Kankare, T. Kravtsov, L.-P. Li, C.-C. Lin, T. B. Lowe, P. Lundqvist, E. A. Magnier, K. Matilainen, P. A. Mazzali, C. McCully, P. Minguez, T. E. Müller-Bravo, M. Newsome, E. Padilla Gonzalez, C. Pellegrino, P. J. Pessi, T. Petrushevska, G. Pignata, R. P. Santos, S. Schulze, S. J. Smartt, I. A. Smith, K. W. Smith, J. Sollerman, S. Srivastav, M. D. Stritzinger, G. Terreran, G. Valerin, R. Wainscoat, S.-Q. Wang, 善钦 王, D. R. Young, L. Galbany, Z. Li, I. Salmaso, S. Zha, 帅 查, J.-M. Bai, 金明 白, B. Wang, 博 王, X.-F. Wang, 晓锋 王, J.-J. Zhang, 居甲 张

Y.-Z. Cai et al 2026 The Astrophysical Journal Letters 1004 .

  • Provider: AAS Journals

Caption: Figure 5.

CSM interaction models with different assumptions for ejecta masses and explosion energies. Left panel: evolution of the shell velocity. Middle panel: CSM density distribution reconstructed from bolometric light curve of SN 2022pda for different ejecta masses and explosion energies. The dotted line shows the rough estimate of CSM optical depth, ρ = 1/(κrsh) with a fiducial value of κ = 0.1 cm2 g−1 representing the scattering opacity of ionized H-poor CSM. Right panel: evolution of pre-explosion mass-loss rate under the assumption of constant CSM expansion velocity vCSM = 1900 km s−1.

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