Eclipses During the 2010 Eruption of the Recurrent Nova U Scorpii

Schaefer, Bradley E.; Pagnotta, Ashley; Lacluyzé, A.; Reichart, D.; Ivarsen, K.; Haislip, J.; Nysewander, M.; Moore, J. P.; Oksanen, A.; Worters, Hannah L.; Sefako, Ramotholo; Mentz, Jaco; Dvorak, Shawn; Gómez, Tomás L.; Harris, B.; Henden, A. A.; Tan, T. G.; Templeton, Matthew R.; Allen, William H.; Monard, B.; Rea, Robert; Roberts, George; Stein, William; Maehara, Hiroyuki; Richards, Thomas; Stockdale, Chris; Krajci, Tom; Sjoberg, George; McCormick, J.; Revnivtsev, M.; Molkov, S.; Suleimanov, V.; Darnley, M. J.; Bode, M. F.; Handler, G.; Lépine, Sébastien; Shara, Michael M.

doi:10.1088/0004-637x/742/2/113

Cited by 28 publications

(35 citation statements)

References 33 publications

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“…However, as our sequence of spectra covers all the major phases of the outburst it is of interest to match the spectral evolution of the nova to the light curve phases that have been identified by Schaefer et al (2011). Figure 1 shows U Sco light curve, the light-curve phases identified by Schaefer and the epochs of our spectroscopic observations.…”

Section: The Broad Emission Lines From the Ejecta And Their Evolutionmentioning

confidence: 97%

“…Before flux calibration the VIS A&A 544, A149 (2012) . The vertical black dashed lines marks the evolutionary phases identified by Schaefer et al (2011), while the red and blue vertical segments marks the epoch of our FEROS and X-Shooter spectroscopic observations, respectively. Each of the light curve evolutionary phases has been marked in the figure itself.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…The U Sco 2010 outburst had an extensive follow-up both from space and ground, and from X-ray to near-infrared (NIR) wavelengths Munari et al 2010;Schaefer et al 2011;Banerjee et al 2010;Yamanaka et al 2010;Diaz et al 2010;Kafka & Williams 2010;Manousakis et al 2010;Ness et al 2012;Orio et al 2010;Osborne et al 2010). …”

Section: Introductionmentioning

confidence: 99%

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U Scorpii 2010 outburst: a new understanding of the binary accretion disk and the secondary star

Mason¹,

Ederoclite²,

Williams³

et al. 2012

A&A

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We present optical and near-infrared (NIR) spectroscopic observations of U Sco 2010 outburst. From the analysis of lines profiles we identify a broad and a narrow component and show that the latter originates from the reforming accretion disk. We show that the accretion resumes shortly after the outburst, on day +8, roughly when the super-soft (SSS) X-ray phase starts. Consequently U Sco SSS phase is fueled (in part or fully) by accretion and should not be used to estimate m rem , the mass of accreted material which has not been ejected during the outburst. In addition, most of the He emission lines, and the He ii lies in particular, form in the accretion flow/disk within the binary and are optically thick, thus preventing an accurate abundance determination.A late spectrum taken in quiescence and during eclipse shows Ca ii H&K, the G-band and Mg ib absorption from the secondary star.However, no other significant secondary star features have been observed at longer wavelengths and in the NIR band.

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Section: The Broad Emission Lines From the Ejecta And Their Evolutionmentioning

confidence: 97%

Section: Observations and Data Reductionmentioning

confidence: 99%

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U Scorpii 2010 outburst: a new understanding of the binary accretion disk and the secondary star

Mason¹,

Ederoclite²,

Williams³

et al. 2012

A&A

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“…X-rays by Swift and the reappearance of the optical eclipses (Schlegel et al 2010d;Schaefer et al 2011). These three events are correlated with the thinning of the expanding nova shell, as described by Hachisu et al (2008): once the shell has become optically thin, it no longer blocks the actual U Sco binary (the two stars and the re-forming accretion disk), and both the X-rays and the eclipses are revealed.…”

Section: Observationsmentioning

confidence: 91%

“…U Sco was observed in all wavelengths from radio to gamma-rays during the 2010 eruption, with detections from IR to soft X-ray. The fast time variations of the light curve are discussed in detail in Schaefer et al (2011); here we focus on the overall shape and spectral energy distribution (SED). We construct daily SEDs and use them to get a new estimate of the total amount of mass ejected during the eruption, m ej , following the method described in Shara et al (2010).…”

Section: U Scorpiimentioning

confidence: 99%

The 2010 Eruption of the Recurrent Nova U Scorpii: The Multi-Wavelength Light Curve

Pagnotta

Schaefer

Clem

et al. 2015

ApJ

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The recurrent nova U Scorpii most recently erupted in 2010. Our collaboration observed the eruption in bands ranging from the Swift XRT and UVOT w2 (193 nm) to K-band (2200 nm), with a few serendipitous observations stretching down to WISE W2 (4600 nm). Considering the time and wavelength coverage, this is the most comprehensively observed nova eruption to date. We present here the resulting multi-wavelength light curve covering the two months of the eruption as well as a few months into quiescence. For the first time, a U Sco eruption has been followed all the way back to quiescence, leading to the discovery of new features in the light curve, including a second, as-yet-unexplained, plateau in the optical and near-infrared. Using this light curve we show that U Sco nearly fits the broken power law decline predicted by Hachisu & Kato, with decline indices of −1.71 ± 0.02 and −3.36 ± 0.14. With our unprecedented multi-wavelength coverage, we construct daily spectral energy distributions and then calculate the total radiated energy of the eruption, E We compare this to the total amount of mass accreted by U Sco before the eruption, to determine whether the white dwarf undergoes a net mass loss or gain, but find that the values for the amount of mass accreted are not precise enough to make a useful comparison. et al. 2010a, 2010bSimonson & MacRobert 2010). The discovery triggered a worldwide invocation of both pre-planned (target of opportunity) and serendipitous observing programs. This was the tenth observed eruption of U Sco (Schaefer 2010), and became by far the best observed nova eruption to date. The eruption began on JD 2455224.32 ± 0.12, peaked on JD 2455224.69 ± 0.07 (T 0 ) at V = 7.5 mag, and returned to quiescence 67 days later (Schaefer et al. 2010b).We present multi-wavelength photometry of the complete eruption obtained by our extensive collaboration of both professional and amateur astronomers. U Sco was observed in all wavelengths from radio to gamma-rays during the 2010 eruption, with detections from IR to soft X-ray. The fast time variations of the light curve are discussed in detail in Schaefer et al. (2011); here we focus on the overall shape and spectral energy distribution (SED). We construct daily SEDs and use them to get a new estimate of the total amount of mass ejected during the eruption, m ej , following the method described in Shara et al. (2010). It is critical to get a good measurement of m ej and compare it to estimates of the total amount of mass accreted during the time interval preceding the eruption to ascertain whether the white dwarf (WD) in the system is gaining or losing mass over the course of the eruption cycle. If the WD, which is already near the Chandrasekhar limit (Hachisu et al. 2000;Thoroughgood et al. 2001), is in fact gaining mass and is composed primarily of carbon and oxygen, it must eventually become a Type Ia supernova (SN Ia). Determining whether RNe can become SNe Ia takes us one step closer to solving the long-standing SN Ia progenitor problem and im...

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The 2010 outburst and pre-outburst optical spectrum of the recurrent nova U Scorpii

Anupama

Kamath

Ramaprakash

et al. 2013

A&A

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Aims. We study the evolution of the recurrent nova U Scorpii during its outburst in 2010. Methods. Optical spectroscopic observations of the nova were obtained during 0.83-162.5 days after outburst maximum. Optical linear polarisation observations were made before the onset of the super soft X-ray source (SSS) phase and during the SSS phase. Radio continuum observations were made in the 1280 MHz band during the early decline phase, and in the 610 MHz band at the onset and end of the SSS phase. We also present optical spectra obtained in the pre-outburst quiescence phase. Results. The overall spectral evolution during the 2010 outburst is similar to the previous outbursts. However, the dense temporal coverage, especially during the early phases, reveals several short term variations not reported previously. The early phase emission line widths indicate extremely high velocities for the nova ejecta, ∼10 000 km s −1 . The line profiles are broad, boxy and structured. Narrow P-Cygni absorptions, at ∼500 km s −1 are seen associated with the He I lines, and also the Ca II, N I and hydrogen lines (at wavelengths >8000 Å) in the spectrum of day 6.83, obtained immediately after an optical flare. This absorption component could be arising in the plasma emitting the Nitrogen lines seen in X-rays, that probably lies outside the binary orbit. Rapid variations are detected in the strength of the 4660 Å N III feature, which shows a significant increase in the line strength on days 8.83 and 13.82, at orbital phases of 0.75 and 0.25, respectively. Instrinsic polarisation is detected just before the onset, and during the SSS phase, with p v ∼ 1.4% during the SSS phase. The flux variations of the N III feature and the intrinsic polarisation are most likely associated with the reforming accretion disc/stream. We estimate the mass of the ejected (hydrogen) shell to be ∼4.6 × 10 −6 M , for a spherical shell geometry. The non-detection of U Sco in the 1280 MHz and 610 MHz radio bands is consistent with the low mass of the nova ejecta, subgiant nature of the secondary, and the distance to the nova.

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Eclipses During the 2010 Eruption of the Recurrent Nova U Scorpii

Abstract: The eruption of the recurrent nova U Scorpii on 28 January 2010 is now the all-time best observed nova event. We report 36,776 magnitudes throughout its

Cited by 28 publications

References 33 publications

U Scorpii 2010 outburst: a new understanding of the binary accretion disk and the secondary star

U Scorpii 2010 outburst: a new understanding of the binary accretion disk and the secondary star

The 2010 Eruption of the Recurrent Nova U Scorpii: The Multi-Wavelength Light Curve

The 2010 outburst and pre-outburst optical spectrum of the recurrent nova U Scorpii

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