The Values of e, h, e/m, and Mp/m

Bond, W. N.

doi:10.1038/127557b0

Cited by 38 publications

(57 citation statements)

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“…The depth of these absorption bands indicate a later spectral type than estimated by Bond & Kasliwal (2012). The fit to our spectrum indicates an M5.0 ± 0.5 III type for the red giant of the system.…”

Section: Iphasj184144mentioning

confidence: 63%

“…This source was previously known as the emission-line star HBHA-0201-01 and variable star NSV 11749. Its symbiotic nature was independently discovered by Bond & Kasliwal (2012) who proposed that it is a symbiotic nova based on the historical light curve that showed an outburst in 1903 followed by a slow photometric decline. An M1-2 III classification of its cool component reddened by 0.75 mag in the visual was determined by these authors from the optical and NIR spectra.…”

Section: Iphasj184144mentioning

confidence: 99%

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IPHAS and the symbiotic stars

Rodriguez-Flores

Corradi

Mampaso

et al. 2014

A&A

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Context. The IPHAS Hα survey provides a rich database to search for emission-line sources in the northern Galactic plane. Aims. We are systematically searching for symbiotic stars in the Milky Way using IPHAS. Our final goal, a complete census of this class of objects in the Galaxy, is a fundamental figure for discussing their overall properties and relevance to other classes of stars. Methods. Candidate symbiotic stars were selected using a refined combination of IPHAS and 2MASS photometric colours. Optical spectroscopy, together with the analysis of their spectral energy distribution in the IR, were obtained to confirm their nature and determine their main properties. Results. Five new symbiotic stars have been confirmed from spectroscopy at the 10.4 m GTC telescope. In one case, confirming the presence of a red giant star required near infrared spectroscopy. In another case, its symbiotic nature was adopted based on the strong similarity of its optical spectrum and spectral energy distribution to those of other genuinely symbiotic stars. The spectral energy distribution of the two S-types found is well fitted by red-giant model atmospheres up to 22 μm without evidence of IR excesses due to dust. In contrast, the three D-types mostly show emission from hot dust with a temperature around 1000 K. We also present the spectroscopic and photometric monitoring of the symbiotic star IPHASJ190832.31+051226.6 that was originally discovered in outburst, and it has now returned to a lower luminosity status. The spectra of thirteen other sources, all classified as young stellar objects except for a new compact planetary nebula, are also presented.Conclusions. The refinement of our discovery method, the completion of the IPHAS survey and photometric calibration, and the start of the twin survey in the south, VPHAS+, provide excellent perspectives for completing a reliable census of symbiotic stars in the Galaxy in the next few years.

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Section: Iphasj184144mentioning

confidence: 63%

Section: Iphasj184144mentioning

confidence: 99%

IPHAS and the symbiotic stars

Rodriguez-Flores

Corradi

Mampaso

et al. 2014

A&A

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“…Early observations between June 29.68 and July 1.68 have detected the nova, but no brightness estimates are available (Bond & Kilmartin 2000), since all images except the first one on June 29.68 show the nova to be saturated (Bond, priv. comm.).…”

Section: Introductionmentioning

confidence: 99%

XMM-Newton observations of Nova LMC 2000

Greiner

Orio²,

Schartel

2003

A&A

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Abstract. We report on three X-ray observations of Nova LMC 2000 with XMM-Newton at 17, 51 and 294 days after the maximum, respectively. X-ray spectral fits show a concordant decrease of the absorbing column and the X-ray luminosity. No supersoft X-ray emission is detected. The mass of the ejected shell is determined to be (less than) 7.5 × 10 −5 M . Though data are sparse, one interesting correlation becomes visible: sources with a long-duration supersoft X-ray phase have shorter orbital periods than those with short or no supersoft X-ray phase. This can be understood considering that (i) enough matter has to be accreted in order to ignite the H burning, and (ii) that H burning ceases when the mass of the remaining material (after shell ejection and burning) drops below a certain limit under which the temperature at the bottom of the envelope is too low for the shell burning to compensate the energy loss from the surface.

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“…From the AAVSO light curve we estimate t 2 < 10 and t 3 < 20 days for this nova. Early spectroscopy of nova LMC 2009a was taken by Orio et al (2009) and Bond et al (2009).…”

Section: Introductionmentioning

confidence: 99%

On the narrow emission line components of the LMC novae 2004 (YY Doradus) and 2009a

Mason

Munari

2014

A&A

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We present early decline spectra of the two Large Magellanic Cloud novae: LMC 2004 (YY Dor) and LMC 2009a and discuss their spectral an line profile evolution with special emphasis on the existence and appearance of a sharp component. We show that the narrow component that characterizes the emission lines in the maximum spectra of nova LMC 2004 originates in the ejecta.The He ii 4686 Å narrow emission which appears at the onset of the nebular phase in both novae is somewhat controversial. Our observations suggest that the corresponding line forming region is physically separated from the rest of the ejecta (the broad line region) and environmentally different. However, the lack of late time observations covering the super-soft source (SSS) phase, the post-SSS phase and the quiescence state does not allow to securely establish any non-ejecta origin/contribution as, instead, in the case of U Sco and KT Eri.

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The Values of e, h, e/m, and Mp/m

Cited by 38 publications

References 0 publications

IPHAS and the symbiotic stars

IPHAS and the symbiotic stars

XMM-Newton observations of Nova LMC 2000

On the narrow emission line components of the LMC novae 2004 (YY Doradus) and 2009a

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