Calamus pauciflorus T. Evans et al. non Ridl. Renamed Calamus oligostachys T. Evans et al.

Evans, Tom; Sengdala, Khamphone; Viengkham, Oulathong V.; Thammavong, Banxa; Dransfield, John

doi:10.2307/4119442

Cited by 112 publications

(174 citation statements)

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“…At optical wavelengths λλ6300, 6363 are found in planetary nebula spectra with λ6300 commonly used for abundance analysis in cool stars. For near-IR wavelengths, detections, or suspicions of detections, have been mentioned for 8446 Å in AG Dra (Iijima et al 1987), and λ11289 (Evans et al 2007). Absorption lines at λλ7771, 7773, 7774 are commonly used in abundance analysis in a variety of stars.…”

Section: Discussionmentioning

confidence: 99%

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The O I] 1641 Å line as a probe of symbiotic star winds

Shore

Wahlgren

2010

A&A

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Aims. The neutral oxygen resonance λ1302 Å line can, if the optical depth is sufficiently high, de-excite by an intercombination transition at λ1641 Å to a metastable state. This has been noted in a number of previous studies but never systematically investigated as a diagnostic of the neutral red giant wind in symbiotic stars and symbiotic-like recurrent novae. Methods. We used archival IUE high resolution, and HST GHRS and STIS medium and high resolution, spectra to study a sample of symbiotic stars. The integrated fluxes were measured, where possible, for the O I λ1302 Å and O I] λ1641 Å lines. Results. The intercombination λ1641 Å line is detected in a substantial number of symbiotic stars with optical depths that give column densities comparable with direct eclipse measures (EG And) and the evolution of the recurrent nova RS Oph 1985 in outburst. In four systems (EG And, Z And, V1016 Cyg, and RR Tel), we find that the O I] variations are strongly correlated with the optical light curve and outburst activity. This transition can also be important for the study of a wide variety of sources in which an ionization-bounded H II region is imbedded in an extensive neutral medium, including active galactic nuclei, and not only for evaluations of extinction.

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Section: Discussionmentioning

confidence: 99%

“…Its radial velocity is consistent with that of the binary system, v rad = −10 km s −1 . To our knowledge, the line O I λ1.12895 μm has only been identified in symbiotic and related star spectra by Evans et al (2007), where it was recorded in post outburst spectra of RS Oph.…”

Section: Notes and Correlationsmentioning

confidence: 99%

The O I] 1641 Å line as a probe of symbiotic star winds

Shore

Wahlgren

2010

A&A

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“…Plotkin et al 2012;Merloni, Heinz, & di Matteo 2003;Falcke, Körding, & Markoff 2004). The VLBA flux density was measured to be 0.22 ± 0.04 mJy at 8.7 GHz, which (assuming a flat spectral index) gives a 5-GHz radio luminosity of (2.1 ± 0.04) × 10 36 erg s −1 , while the X-ray luminosity as measured by SWIFT is 5.6 +2.4 −1.9 × 10 39 erg s −1 (Evans et al 2017). The radio spectral index is consistent with being flat or slightly negative (as can be seen from the ATCA results shown in Table 9); the results are insensitive to small variations in this parameter.…”

Section: The Host Galaxymentioning

confidence: 99%

Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes

Andreoni

Ackley

Cooke

et al. 2017

Publ. Astron. Soc. Aust.

184

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The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early-to late-time multi-wavelength observations, including optical imaging and spectroscopy, midinfrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source emission cooled from approximately 6 400 K to 2 100 K over a 7-d period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (∼2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor.

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“…Kellogg et al 1979; Anderson et al 1980; Orheim & 118 Elverhøi, 1981;Domack, 1982;Haase, 1986;Kennedy & Anderson, 1989 Pudsey et al 1994;Larter & Vanneste, 1995;O'Brien et al 1999;Shipp et al 1999; Canals 123 et al 2000 Canals 123 et al , 2002 Canals 123 et al , 2003Anderson & Shipp, 2001;Wellner et al 2001;Ó Cofaigh et al 2002 Ó Cofaigh et al , 124 2003 Ó Cofaigh et al , 2005a Lowe & Anderson, 2003; Dowdeswell et al 2004a,b;Evans et al 2004Evans et al , 2005 recently been demonstrated (Padman et al, 2010).…”

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confidence: 99%

Antarctic palaeo-ice streams

Livingstone

Cofaigh

Stokes

et al. 2012

Earth-Science Reviews

180

183

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We review the geomorphological, sedimentological and chronological evidence for palaeo- palaeo-ice streams to be classified into discrete retreat styles and the controls on grounding-21 line retreat to be investigated. Such analysis highlights the important impact of internal 22 factors on ice stream dynamics, such as bed characteristics and slope, and drainage basin size. 23Whilst grounding-line retreat may be triggered, and to some extent paced, by external 24 (atmospheric and oceanic) forcing, the individual characteristics of each ice stream will 25 modulate the precise timing and rate of retreat through time. ). The ability to directly observe the beds of palaeo-ice streams has also allowed 65 scientists to glean important spatial and temporal information on the processes that occurred 66 at the ice-bed interface and on the evolution of palaeo-ice streams throughout their glacial 67 history. 68Over the last two decades, there has been a burgeoning interest in marine palaeo-ice streams, and the timing and rate of deglaciation (e.g. Wellner et al. 2001;Canals et al., 2000; Lowe & 73 Anderson, 2002;Ó Cofaigh et al. 2002;Graham et al. 2009 115The first glacimarine investigations in Antarctica utilised echosounder data, till petrographic 116 studies and seismic data to reconstruct the expansion of grounded ice across the continental 117 shelf during the last glaciation (e.g. Kellogg et al. 1979; Anderson et al. 1980; Orheim & 118 Elverhøi, 1981;Domack, 1982;Haase, 1986;Kennedy & Anderson, 1989 Pudsey et al. 1994;Larter & Vanneste, 1995;O'Brien et al. 1999;Shipp et al. 1999; Canals 123 et al. 2000 Canals 123 et al. , 2002 Canals 123 et al. , 2003Anderson & Shipp, 2001;Wellner et al. 2001;Ó Cofaigh et al. 2002 Ó Cofaigh et al. , 124 2003 Ó Cofaigh et al. , 2005a Lowe & Anderson, 2003; Dowdeswell et al. 2004a,b;Evans et al. 2004Evans et al. , 2005 recently been demonstrated (Padman et al., 2010). 132In O'Brien et al. 1999O'Brien et al. , 2007 Table 2 provides a synthesis of the key physiographic data of each palaeo-ice stream in our 215 new inventory (see Fig. 1 and (ten Brink & Schneider, 1995). 228It is also apparent from 248The majority of the Antarctic palaeo-ice streams retreated across reverse slopes ( 2010) is suggested to relate to the much smaller size of its drainage basin (10,000-100,000 269 km 2 ), which is likely to have been much more sensitive to external and internal forcing. East Antarctic Peninsula, has also been associated with a change in basal processes (from 327 9 basal sliding to deformation) and an increase in ice velocity (Reinardy et al. 2011b The geometry of the basal reflector underlying the acoustically transparent unit ranges from 363 smooth and flat to irregular and undulating ( shelf (Pudsey et al. 1994Licht et al. 1996Licht et al. , 1998Licht et al. , 1999 between this bedrock and unconsolidated sediment further out on the shelf (Fig. 4c and Table 493 3) (Anderson et al. 2001; Camerlenghi et al. 2001;Wellner et al. 2001Wellner et al. , 2006...

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Calamus pauciflorus T. Evans et al. non Ridl. Renamed Calamus oligostachys T. Evans et al.

Cited by 112 publications

References 1 publication

The O I] 1641 Å line as a probe of symbiotic star winds

The O I] 1641 Å line as a probe of symbiotic star winds

Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes

Antarctic palaeo-ice streams

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