Variable stars in the Small Magellanic Cloud

Gaposchkin, Cecilia Helena Payne; Gaposchkin, Sergei

doi:10.5479/si.00810231.9.1

Cited by 69 publications

(49 citation statements)

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“…For this Cepheid, we compiled photometric data taken during 1970-1976 from Madore (1975) and van Genderen (1983 data from the ASAS catalog (see Figure 7). This result is confirmed by a measured period of 87.63 days in Payne-Gaposchkin & Gaposchkin (1966) and 85.2 days by Moffett et al (1998), firmly establishing HV829 as a Cepheid on its second crossing. No other Cepheid in our sample exhibited a measurable period change.…”

Section: Using Ulp Cepheids To Probe the Evolutionary Models Of Massisupporting

confidence: 69%

USING ULTRA LONG PERIOD CEPHEIDS TO EXTEND THE COSMIC DISTANCE LADDER TO 100 Mpc AND BEYOND

Bird

Stanek

Prieto

2009

ApJ

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We examine the properties of 18 long period (80-210 days) and very luminous (median absolute magnitude of M I = −7.86 and M V = −6.97) Cepheids to see if they can serve as a useful distance indicator. We find that these Ultra Long Period (ULP) Cepheids have a relatively shallow period-luminosity (PL) relation, so in fact they are more "standard candle" like than classical Cepheids. In the reddening-free Wesenheit index, the slope of the ULP PL relation is consistent with zero. The scatter of our sample about the W I PL relation is 0.23 mag, approaching that of classical Cepheids and Type Ia Supernovae. We expect this scatter to decrease as bigger and more uniform samples of ULP Cepheids are obtained. We also measure a nonzero period derivative for one ULP Cepheid (SMC HV829) and use the result to probe evolutionary models and mass loss of massive stars. ULP Cepheids' main advantage over classical Cepheids is that they are more luminous, and as such show great potential as stellar distance indicators to galaxies up to 100 Mpc and beyond.

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Section: Using Ulp Cepheids To Probe the Evolutionary Models Of Massisupporting

confidence: 69%

USING ULTRA LONG PERIOD CEPHEIDS TO EXTEND THE COSMIC DISTANCE LADDER TO 100 Mpc AND BEYOND

Bird

Stanek

Prieto

2009

ApJ

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“…They are population I, relatively massive (M > 4 M ) giant stars obeying the famous period-luminosity (PL) relationship discovered in the Magellanic Clouds by Henrietta Leavitt in 1908 ([18]). Figure 1 shows how many classical Cepheids in the Magellanic Clouds have been known from the beginning of the twentieth century, starting from 16 Cepheids 1 discovered by Leavitt ([18]), through several review and catalog papers summarizing the number of Cepheids known in those days ( [25,26,36,37]), the first catalogs of Cepheids in the Magellanic Clouds released by the MACHO and OGLE-II projects in 1999 ( [5,60,61]), ending with a real breakthrough that was made in recent years by OGLE-III ( [40,44]) and OGLE-IV projects ( [53]). Currently, we almost reached the maximum value of this distribution.…”

Section: Classical Cepheidsmentioning

confidence: 99%

“…In the next sections we present respectively classical Cepheids, RR Lyrae stars, type II Cepheids, anomalous Cepheids, long-period variables, and other pulsating stars. [18], [19], [36], [37], [25], [26], [5], [60], [61], [40], [44], [53].…”

Section: Introductionmentioning

confidence: 99%

The impact of large-scale, long-term optical surveys on pulsating star research

Soszyński

2017

EPJ Web Conf.

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Abstract. The era of large-scale photometric variability surveys began a quarter of a century ago, when three microlensing projects -EROS, MACHO, and OGLE -started their operation. These surveys initiated a revolution in the field of variable stars and in the next years they inspired many new observational projects. Large-scale optical surveys multiplied the number of variable stars known in the Universe. The huge, homogeneous and complete catalogs of pulsating stars, such as Cepheids, RR Lyrae stars, or long-period variables, offer an unprecedented opportunity to calibrate and test the accuracy of various distance indicators, to trace the three-dimensional structure of the Milky Way and other galaxies, to discover exotic types of intrinsically variable stars, or to study previously unknown features and behaviors of pulsators. We present historical and recent findings on various types of pulsating stars obtained from the optical large-scale surveys, with particular emphasis on the OGLE project which currently offers the largest photometric database among surveys for stellar variability.

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“…However, the resonance out-of-plane from the variation of the node may have serious errors if only linear analysis is used as in Gaposchkin andLambeck, 1970 andGaposchkin, 1973. Table 1 presents these maximum linear and total variations of the node for the 21 satellite orbits (excluding ERTS) used in the Smithsonian Standard Earth's (see also Gaposchkin, 1966). Almost half show more than 10% change when the indirect effects are included.…”

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confidence: 99%

Effect of resonance-oblateness coupling on a satellite orbit

Wagner¹

1975

J. Geophys. Res.

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Second‐order effects of the coupling between geopotential resonance and oblateness on a satellite orbit are calculated. These effects arise from the interaction of resonance with the secular changes of the orbit's node, perigee, and mean anomaly. They have the same period and phase as first‐order resonance perturbations. But their amplitudes are proportional to the square of the period and dominate the first‐order effects as the orbit becomes commensurate. A striking example of this coupling is seen in the 18‐day resonance variation of the node of the orbit of the first earth resources technology satellite. Analysis of this 1 arc sec (31 m) variation yields a strong fourteenth‐order constraint to the geopotential field for odd degree terms. This constraint (lumped coefficient) is poorly predicted by most current models.

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Variable stars in the Small Magellanic Cloud

Cited by 69 publications

References 0 publications

USING ULTRA LONG PERIOD CEPHEIDS TO EXTEND THE COSMIC DISTANCE LADDER TO 100 Mpc AND BEYOND

USING ULTRA LONG PERIOD CEPHEIDS TO EXTEND THE COSMIC DISTANCE LADDER TO 100 Mpc AND BEYOND

The impact of large-scale, long-term optical surveys on pulsating star research

Effect of resonance-oblateness coupling on a satellite orbit

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