Report
View in EDS

Inflows, Outflows, and a Giant Donor in the Remarkable Recurrent Nova M31N 2008-12a? - Hubble Space Telescope Photometry of the 2015 Eruption

Bibliographic Details
Title: Inflows, Outflows, and a Giant Donor in the Remarkable Recurrent Nova M31N 2008-12a? - Hubble Space Telescope Photometry of the 2015 Eruption
Authors: Darnley, M. J., Hounsell, R., Godon, P., Perley, D. A., Henze, M., Kuin, N. P. M., Williams, B. F., Williams, S. C., Bode, M. F., Harman, D. J., Hornoch, K., Link, M., Ness, J. -U., Ribeiro, V. A. R. M., Sion, E. M., Shafter, A. W., Shara, M. M.
Publication Year: 2017
Collection: Astrophysics
Subject Terms: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
More Details: The recurrent nova M31N 2008-12a experiences annual eruptions, contains a near-Chandrasekhar mass white dwarf, and has the largest mass accretion rate in any nova system. In this paper, we present Hubble Space Telescope (HST) WFC3/UVIS photometry of the late decline of the 2015 eruption. We couple these new data with archival HST observations of the quiescent system and Keck spectroscopy of the 2014 eruption. The late-time photometry reveals a rapid decline to a minimum luminosity state, before a possible recovery / re-brightening in the run-up to the next eruption. Comparison with accretion disk models supports the survival of the accretion disk during the eruptions, and uncovers a quiescent disk mass accretion rate of the order of $10^{-6}\,M_\odot\,\mathrm{yr}^{-1}$, which may rise beyond $10^{-5}\,M_\odot\,\mathrm{yr}^{-1}$ during the super-soft source phase - both of which could be problematic for a number of well-established nova eruption models. Such large accretion rates, close to the Eddington limit, might be expected to be accompanied by additional mass loss from the disk through a wind and even collimated outflows. The archival HST observations, combined with the disk modeling, provide the first constraints on the mass donor; $L_\mathrm{donor}=103^{+12}_{-11}\,L_\odot$, $R_\mathrm{donor}=14.14^{+0.46}_{-0.47}\,R_\odot$, and $T_\mathrm{eff, donor}=4890\pm110$ K, which may be consistent with an irradiated M31 red-clump star. Such a donor would require a system orbital period $\gtrsim5$ days. Our updated analysis predicts that the M31N 2008-12a WD could reach the Chandrasekhar mass in < 20 kyr.
Comment: 20 pages, 8 figures, 5 tables, accepted for publication in The Astrophysical Journal
Document Type: Working Paper
DOI: 10.3847/1538-4357/aa9062
Access URL: http://arxiv.org/abs/1709.10145
Accession Number: edsarx.1709.10145
Database: arXiv
FullText Text:
  Availability: 0
CustomLinks:
  – Url: http://arxiv.org/abs/1709.10145
    Name: EDS - Arxiv
    Category: fullText
    Text: View this record from Arxiv
    MouseOverText: View this record from Arxiv
  – Url: https://resolver.ebsco.com/c/xy5jbn/result?sid=EBSCO:edsarx&genre=article&issn=&ISBN=&volume=&issue=&date=20170928&spage=&pages=&title=Inflows, Outflows, and a Giant Donor in the Remarkable Recurrent Nova M31N 2008-12a? - Hubble Space Telescope Photometry of the 2015 Eruption&atitle=Inflows%2C%20Outflows%2C%20and%20a%20Giant%20Donor%20in%20the%20Remarkable%20Recurrent%20Nova%20M31N%202008-12a%3F%20-%20Hubble%20Space%20Telescope%20Photometry%20of%20the%202015%20Eruption&aulast=Darnley%2C%20M.%20J.&id=DOI:10.3847/1538-4357/aa9062
    Name: Full Text Finder (for New FTF UI) (s8985755)
    Category: fullText
    Text: Find It @ SCU Libraries
    MouseOverText: Find It @ SCU Libraries
Header DbId: edsarx
DbLabel: arXiv
An: edsarx.1709.10145
RelevancyScore: 971
AccessLevel: 3
PubType: Report
PubTypeId: report
PreciseRelevancyScore: 970.66552734375
IllustrationInfo
Items – Name: Title
  Label: Title
  Group: Ti
  Data: Inflows, Outflows, and a Giant Donor in the Remarkable Recurrent Nova M31N 2008-12a? - Hubble Space Telescope Photometry of the 2015 Eruption
– Name: Author
  Label: Authors
  Group: Au
  Data: &lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Darnley%2C+M%2E+J%2E%22&quot;&gt;Darnley, M. J.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Hounsell%2C+R%2E%22&quot;&gt;Hounsell, R.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Godon%2C+P%2E%22&quot;&gt;Godon, P.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Perley%2C+D%2E+A%2E%22&quot;&gt;Perley, D. A.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Henze%2C+M%2E%22&quot;&gt;Henze, M.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Kuin%2C+N%2E+P%2E+M%2E%22&quot;&gt;Kuin, N. P. M.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Williams%2C+B%2E+F%2E%22&quot;&gt;Williams, B. F.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Williams%2C+S%2E+C%2E%22&quot;&gt;Williams, S. C.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Bode%2C+M%2E+F%2E%22&quot;&gt;Bode, M. F.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Harman%2C+D%2E+J%2E%22&quot;&gt;Harman, D. J.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Hornoch%2C+K%2E%22&quot;&gt;Hornoch, K.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Link%2C+M%2E%22&quot;&gt;Link, M.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Ness%2C+J%2E+-U%2E%22&quot;&gt;Ness, J. -U.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Ribeiro%2C+V%2E+A%2E+R%2E+M%2E%22&quot;&gt;Ribeiro, V. A. R. M.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Sion%2C+E%2E+M%2E%22&quot;&gt;Sion, E. M.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Shafter%2C+A%2E+W%2E%22&quot;&gt;Shafter, A. W.&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;AR&quot; term=&quot;%22Shara%2C+M%2E+M%2E%22&quot;&gt;Shara, M. M.&lt;/searchLink&gt;
– Name: DatePubCY
  Label: Publication Year
  Group: Date
  Data: 2017
– Name: Subset
  Label: Collection
  Group: HoldingsInfo
  Data: Astrophysics
– Name: Subject
  Label: Subject Terms
  Group: Su
  Data: &lt;searchLink fieldCode=&quot;DE&quot; term=&quot;%22Astrophysics+-+High+Energy+Astrophysical+Phenomena%22&quot;&gt;Astrophysics - High Energy Astrophysical Phenomena&lt;/searchLink&gt;&lt;br /&gt;&lt;searchLink fieldCode=&quot;DE&quot; term=&quot;%22Astrophysics+-+Solar+and+Stellar+Astrophysics%22&quot;&gt;Astrophysics - Solar and Stellar Astrophysics&lt;/searchLink&gt;
– Name: Abstract
  Label: Description
  Group: Ab
  Data: The recurrent nova M31N 2008-12a experiences annual eruptions, contains a near-Chandrasekhar mass white dwarf, and has the largest mass accretion rate in any nova system. In this paper, we present Hubble Space Telescope (HST) WFC3/UVIS photometry of the late decline of the 2015 eruption. We couple these new data with archival HST observations of the quiescent system and Keck spectroscopy of the 2014 eruption. The late-time photometry reveals a rapid decline to a minimum luminosity state, before a possible recovery / re-brightening in the run-up to the next eruption. Comparison with accretion disk models supports the survival of the accretion disk during the eruptions, and uncovers a quiescent disk mass accretion rate of the order of $10^{-6}\,M_\odot\,\mathrm{yr}^{-1}$, which may rise beyond $10^{-5}\,M_\odot\,\mathrm{yr}^{-1}$ during the super-soft source phase - both of which could be problematic for a number of well-established nova eruption models. Such large accretion rates, close to the Eddington limit, might be expected to be accompanied by additional mass loss from the disk through a wind and even collimated outflows. The archival HST observations, combined with the disk modeling, provide the first constraints on the mass donor; $L_\mathrm{donor}=103^{+12}_{-11}\,L_\odot$, $R_\mathrm{donor}=14.14^{+0.46}_{-0.47}\,R_\odot$, and $T_\mathrm{eff, donor}=4890\pm110$ K, which may be consistent with an irradiated M31 red-clump star. Such a donor would require a system orbital period $\gtrsim5$ days. Our updated analysis predicts that the M31N 2008-12a WD could reach the Chandrasekhar mass in &lt; 20 kyr.&lt;br /&gt;Comment: 20 pages, 8 figures, 5 tables, accepted for publication in The Astrophysical Journal
– Name: TypeDocument
  Label: Document Type
  Group: TypDoc
  Data: Working Paper
– Name: DOI
  Label: DOI
  Group: ID
  Data: 10.3847/1538-4357/aa9062
– Name: URL
  Label: Access URL
  Group: URL
  Data: &lt;link linkTarget=&quot;URL&quot; linkTerm=&quot;http://arxiv.org/abs/1709.10145&quot; linkWindow=&quot;_blank&quot;&gt;http://arxiv.org/abs/1709.10145&lt;/link&gt;
– Name: AN
  Label: Accession Number
  Group: ID
  Data: edsarx.1709.10145
PLink https://login.libproxy.scu.edu/login?url=https://search.ebscohost.com/login.aspx?direct=true&site=eds-live&scope=site&db=edsarx&AN=edsarx.1709.10145
RecordInfo BibRecord:
  BibEntity:
    Identifiers:
      – Type: doi
        Value: 10.3847/1538-4357/aa9062
    Subjects:
      – SubjectFull: Astrophysics - High Energy Astrophysical Phenomena
        Type: general
      – SubjectFull: Astrophysics - Solar and Stellar Astrophysics
        Type: general
    Titles:
      – TitleFull: Inflows, Outflows, and a Giant Donor in the Remarkable Recurrent Nova M31N 2008-12a? - Hubble Space Telescope Photometry of the 2015 Eruption
        Type: main
  BibRelationships:
    HasContributorRelationships:
      – PersonEntity:
          Name:
            NameFull: Darnley, M. J.
      – PersonEntity:
          Name:
            NameFull: Hounsell, R.
      – PersonEntity:
          Name:
            NameFull: Godon, P.
      – PersonEntity:
          Name:
            NameFull: Perley, D. A.
      – PersonEntity:
          Name:
            NameFull: Henze, M.
      – PersonEntity:
          Name:
            NameFull: Kuin, N. P. M.
      – PersonEntity:
          Name:
            NameFull: Williams, B. F.
      – PersonEntity:
          Name:
            NameFull: Williams, S. C.
      – PersonEntity:
          Name:
            NameFull: Bode, M. F.
      – PersonEntity:
          Name:
            NameFull: Harman, D. J.
      – PersonEntity:
          Name:
            NameFull: Hornoch, K.
      – PersonEntity:
          Name:
            NameFull: Link, M.
      – PersonEntity:
          Name:
            NameFull: Ness, J. -U.
      – PersonEntity:
          Name:
            NameFull: Ribeiro, V. A. R. M.
      – PersonEntity:
          Name:
            NameFull: Sion, E. M.
      – PersonEntity:
          Name:
            NameFull: Shafter, A. W.
      – PersonEntity:
          Name:
            NameFull: Shara, M. M.
    IsPartOfRelationships:
      – BibEntity:
          Dates:
            – D: 28
              M: 09
              Type: published
              Y: 2017
ResultId 1