Long-term photometry and periods for 261 nearby pulsating M giants

Tabur, V.; Bedding, Timothy R.; Kiss, L. L.; Moon, T. T.; Szeidl, B.; Kjeldsen, H.

doi:10.1111/j.1365-2966.2009.15588.x

Cited by 30 publications

(36 citation statements)

References 49 publications

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“…Many giants later than M6 are brighter than the tip of the RGB (e.g. Tabur et al 2009a), which has observationally been set at M K =−6.85 (Tabur, Kiss & Bedding 2009b), and so most M8 III giants are likely on the AGB.…”

Section: Resultsmentioning

confidence: 99%

Fast X-ray transients towards the Galactic bulge with the Rossi X-ray Timing Explorer

Smith¹,

Markwardt²,

Swank³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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In X‐ray binaries, rapid variability in X‐ray flux of greater than an order of magnitude on time‐scales of a day or less appears to be a signature of wind accretion from a supergiant companion. When the variability takes the form of rare, brief, bright outbursts with only faint emission between them, the systems are called supergiant fast X‐ray transients (SFXTs). We present data from twice‐weekly scans of the Galactic bulge by the Rossi X‐ray Timing Explorer that allow us to compare the behaviour of known SFXTs and possible SFXT candidates with the persistently bright supergiant X‐ray binary 4U 1700−377. We independently confirm the orbital periods reported by other groups for SFXTs SAX J1818.6−1703 and IGR J17544−2619. The new data do not independently reproduce the orbital period reported for XTE J1739−302, but slightly improve the significance of the original result when the data are combined. The bulge source XTE J1743−363 shows a combination of fast variability and a long‐term decline in activity, the latter behaviour not being characteristic of supergiant X‐ray binaries. A far‐red spectrum of the companion suggests that it is a symbiotic neutron star binary rather than a high‐mass binary, and the reddest known of this class: the spectral type is approximately M8 III.

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Section: Resultsmentioning

confidence: 99%

Fast X-ray transients towards the Galactic bulge with the Rossi X-ray Timing Explorer

Smith¹,

Markwardt²,

Swank³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…To collect K-band apparent magnitudes, we followed the process described in Tabur et al (2009) and searched the available NIR catalogues: Catalogue of Infrared Observations (CIO, Gezari et al 1999) and Diffuse Infrared Background Experiment archive (DIRBE Catalogue of Stellar Photometry in Johnson's, Ducati 2002). We used the Gezari K-band magnitudes for 43 stars and the Two Micron All Sky Survey (2MASS) catalogue (Cutri et al 2003) for three objects (CK Car, AO Cru and PP Per).…”

Section: Apparent K-band Magnitudesmentioning

confidence: 99%

The period–luminosity relation of red supergiants with Gaia DR2

Chatys

Bedding

Murphy

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We revisit the K -band period-luminosity (P-L) relations of Galactic red supergiants using Gaia Data Release 2 parallaxes and up to 70 yr of photometry from AAVSO and ASAS campaigns. In addition, we examine 206 LMC red supergiants using 50 yr of photometric data from the Digitised Harvard Astronomical Plate Collection. We identified periods by computing power spectra and calculated the period-luminosity relations of our samples and compared them with the literature. Newly available data tighten the P-L relations substantially. Identified periods form two groups: one with periods of 300-1000 days, corresponding to pulsations, and another with Long Secondary Periods between 1000 and 8000 days. Among the 48 Galactic objects we find shorter periods in 25 stars and long secondary periods in 23 stars. In the LMC sample we identify 85 and 94 red supergiants with shorter and long secondary periods, respectively. The P-L relation of the Galactic red supergiants is in agreement with the red supergiants in both, the Large Magellanic Cloud and the Andromeda Galaxy. We find no clear continuity between the known red giant period-luminosity sequences, and the red supergiant sequences investigated here.

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“…This should be very similar to the light curve amplitude at the peak of the star's SED. Light curves from the Diffuse Infrared Background Experiment (DIRBE), although of poor signal-to-noise (Price et al 2010), show the amplitude of EU Del rises from ∼0.05 mag at 4.9 µm to ∼0.1 mag at 2.2 µm (see also Tabur et al 2009). The amplitude increases further to ∼0.45 mag in the Hipparcos data at 0.53 µm (van Leeuwen 2007).…”

Section: A Pulsation-driven Wind?mentioning

confidence: 99%

EU Del: exploring the onset of pulsation-driven winds in giant stars

McDonald

Sloan

Lagadec

et al. 2016

Mon. Not. R. Astron. Soc.

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We explore the wind-driving mechanism of giant stars through the nearby (117 pc), intermediate-luminosity (L ≈ 1600 L ⊙ ) star EU Del (HIP 101810, HD 196610). APEX observations of the CO (3-2) and (2-1) transitions are used to derive a wind velocity of 9.51 ± 0.02 km s −1 , a 12 C/ 13 C ratio of 14 +9−4 , and a mass-loss rate of a few × 10 −8 M ⊙ yr −1 . From published spectra, we estimate that the star has a metallicity of [Fe/H] = -0.27 ± ∼0.30 dex. The star's dusty envelope lacks a clear 10-µm silicate feature, despite the star's oxygen-rich nature. Radiative transfer modelling cannot fit a wind acceleration model which relies solely on radiation pressure on condensing dust. We compare our results to VY Leo (HIP 53449), a star with similar temperature and luminosity, but different pulsation properties. We suggest the much stronger mass loss from EU Del may be driven by long-period stellar pulsations, due to its potentially lower mass. We explore the implications for the mass-loss rate and wind velocities of other stars.

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Long-term photometry and periods for 261 nearby pulsating M giants

Cited by 30 publications

References 49 publications

Fast X-ray transients towards the Galactic bulge with the Rossi X-ray Timing Explorer

Fast X-ray transients towards the Galactic bulge with the Rossi X-ray Timing Explorer

The period–luminosity relation of red supergiants with Gaia DR2

EU Del: exploring the onset of pulsation-driven winds in giant stars

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