Corrosive damage to N-1 alloy by iodine during creep (stress rupture) tests

Artyukhina, L. L.; Новиков, В. В.; Pirogov, E. N.; Makarov, V. A.

doi:10.1007/bf02045020

Cited by 4 publications

(5 citation statements)

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“…Praesepe was first investigated by Klein Wassink (1924) andKlein Wassink (1927) with subsequent studies by Johnson (1952), Artyukhina (1966), Crawford & Barnes (1969), Artyukhina (1973), Upgren et al (1979), Weis (1981), Hauck (1981), and Jones & Cudworth (1983) before exploring lower mass members (Mermilliod et al 1990;Jones & Stauffer 1991;Gatewood & de Jonge 1994;Williams et al 1994), binarity (Bolte 1991;Mermilliod et al 1994;Bouvier et al 2001;Patience et al 2002;Gillen et al 2017;Hillenbrand et al 2018), lithium (King & Hiltgen 1996;Cummings et al 2017), and its luminosity/mass functions (Lee et al 1997;Kraus & Hillenbrand 2007;Boudreault et al 2012). The advent of photographic plates with several epochs of observations led to a exhaustive census of stellar members over a large area down to 0.1 M (Hambly et al 1995).…”

Section: The Praesepe Clustermentioning

confidence: 99%

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A 5D view of the α Per, Pleiades, and Praesepe clusters

Lodieu

Garrido

Smart

et al. 2019

A&A

109

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Aims. Our scientific goal is to provide revised membership lists of the α Per, Pleiades, and Praesepe clusters exploiting the second data release of Gaia and produce five-dimensional maps (α, δ, π, µ α cosδ, µ δ ) of these clusters. Methods. We implemented the kinematic method combined with the statistical treatment of parallaxes and proper motions to identify astrometric member candidates of three of the most nearby and best studied open clusters in the sky. Results. We cross-correlated the Gaia catalogue with large-scale public surveys to complement the astrometry of Gaia with multiband photometry from the optical to the mid-infrared. We identified 517, 1248, and 721 bona-fide astrometric member candidates inside the tidal radius of the α Per, the Pleiades, and Praesepe, respectively. We cross-matched our final samples with catalogues from previous surveys to address the level of completeness. We update the main physical properties of the clusters, including mean distance and velocity as well as core, half-mass, and tidal radii. We infer updated ages from the white dwarf members of the Pleiades and Praesepe. We derive the luminosity and mass functions of the three clusters and compare them to the field mass function. We compute the positions in space of all member candidates in the three regions to investigate their distribution in space. Conclusions. We provide updated distances and kinematics for the three clusters. We identify a list of members in the α Per, Pleiades, and Praesepe clusters from the most massive stars all the way down into the hydrogen-burning limit with a higher confidence and better astrometry than previous studies. We produce complete 5D maps of stellar and substellar bona-fide members in these three regions. The photometric sequences derived in several colour-magnitude diagrams represent benchmark cluster sequences at ages from 90 to 600 Myr. We note the presence of a stream around the Pleiades cluster extending up to 40 pc from the cluster centre.

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Section: The Praesepe Clustermentioning

confidence: 99%

“…The core of the cluster was estimated to 1.3 degrees in radius (Artyukhina 1972;Kharchenko et al 2005), translating into about 4 pc at the distance of the cluster. The core radius is the radius at which the brightness drops to one-half the central value and is equal to 0.64 times the Plummer radius (Plummer 1915).…”

Section: Member Candidates In α Permentioning

confidence: 99%

A 5D view of the α Per, Pleiades, and Praesepe clusters

Lodieu

Garrido

Smart

et al. 2019

A&A

109

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“…As the basis of this catalog, we adopt the Stauffer et al (2007) list of Pleiades members. This compilation includes 1416 candidate members identified by others over more than 80 years (e.g., by Trumpler 1921;Artyukhina 1969;van Leeuwen et al 1986;Deacon & Hambly 2004).…”

Section: Membership Catalogmentioning

confidence: 99%

Why Are Rapidly Rotating M Dwarfs in the Pleiades So (Infra)red? New Period Measurements Confirm Rotation-Dependent Color Offsets From the Cluster Sequence

Covey

Agüeros

Law

et al. 2016

ApJ

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Stellar rotation periods (P rot ) measured in open clusters have proved to be extremely useful for studying stars' angular momentum content and rotationally driven magnetic activity, which are both age-and mass-dependent processes. While P rot measurements have been obtained for hundreds of solar-mass members of the Pleiades, measurements exist for only a few low-mass (<0.5 M ) members of this key laboratory for stellar evolution theory. To fill this gap, we report P rot for 132 low-mass Pleiades members (including nearly 100 with M ≤ 0.45 M ), measured from photometric monitoring of the cluster conducted by the Palomar Transient Factory in late 2011 and early 2012. These periods extend the portrait of stellar rotation at 125 Myr to the lowest-mass stars and re-establish the Pleiades as a key benchmark for models of the transport and evolution of stellar angular momentum. Combining our new P rot with precise BV IJHK photometry reported by Stauffer et al. and Kamai et al., we investigate known anomalies in the photometric properties of K and M Pleiades members. We confirm the correlation detected by Kamai et al. between a star's P rot and position relative to the main sequence in the cluster's color-magnitude diagram. We find that rapid rotators have redder (V − K) colors than slower rotators at the same V , indicating that rapid and slow rotators have different binary frequencies and/or photospheric properties. We find no difference in the photometric amplitudes of rapid and slow rotators, indicating that asymmetries in the longitudinal distribution of starspots do not scale grossly with rotation rate.

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“…Based on proper motions of 814 stars in the cluster area, Lengauer (1937) identified 39 cluster members. Later, Artyukhina & Kholopov (1966) investigated the cluster members. Based on a B versus B − V diagram, obtained from the data of Mianes & Daguillon (1956), as well as Becker & Stock (1954), the authors found 86 members.…”

Section: The Open Stellar Cluster Ngc 7243mentioning

confidence: 99%

Search for transiting exoplanets and variable stars in the open cluster NGC 7243

et al. 2016

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We report results of the first five observing campaigns for the open stellar cluster NGC 7243 in the frame of project Young Exoplanet Transit Initiative (YETI). The project focuses on the monitoring of young and nearby stellar clusters, with the aim to detect young transiting exoplanets and to study other variability phenomena on time-scales from minutes to years. After five observing campaigns and additional observations during 2013 and 2014, a clear and repeating transit-like signal was detected in the light curve of J221550.6+495611. Furthermore, we detected and analysed 37 new eclipsing binary stars in the studied region. The best fit parameters and light curves of all systems are given. Finally, we detected and analysed 26 new, presumably pulsating variable stars in the studied region. The follow-up investigation of these objects, including spectroscopic measurements of the exoplanet candidate, is currently planned.

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Corrosive damage to N-1 alloy by iodine during creep (stress rupture) tests

Cited by 4 publications

References 0 publications

A 5D view of the α Per, Pleiades, and Praesepe clusters

A 5D view of the α Per, Pleiades, and Praesepe clusters

Why Are Rapidly Rotating M Dwarfs in the Pleiades So (Infra)red? New Period Measurements Confirm Rotation-Dependent Color Offsets From the Cluster Sequence

Search for transiting exoplanets and variable stars in the open cluster NGC 7243

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