The stellar activity-rotation relationship revisited: Dependence of saturated and non-saturated X-ray emission regimes on stellar mass for late-type dwarfs ?

By N. Pizzolato, A. Maggio, G. Micela, S. Sciortino, P. Ventura. 2003

630 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4b85825be1be9e5e2938f37cdcd43bb5c97b10b0

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Citations in the corpus

A VOLUME-LIMITED SAMPLE OF 63 M7–M9.5 DWARFS. II. ACTIVITY, MAGNETISM, AND THE FADE OF THE ROTATION-DOMINATED DYNAMO (2009, background): “The M dwarfs occupy the range between −3.0 and −1.4 in Rossby number, which is well within the saturation regime (see, e.g., Pizzolato et al. 2003).”
GU Bootis: A New 0.6 M☉ Detached Eclipsing Binary (2005, background): “Young low-mass stars are known to be very active because they are generally fast rotators (e.g., Pizzolato et al. 2003).”
Observations of Cool-Star Magnetic Fields (2012, background): “Investigating a rich sample of X-ray, coronal, activity measurements, Pizzolato et al. (2003) were able to show a well-defined rotation-activity relation connecting normalized X-ray luminosity and Rossby number.”
THE Hα EMISSION OF NEARBY M DWARFS AND ITS RELATION TO STELLAR ROTATION (2016, methodology): “This has been demonstrated using coronal (x-ray) emission (e.g. Pallavicini et al. 1981; Vilhu 1984; Pizzolato et al. 2003; Wright et al. 2011), chromospheric (Hα and Ca II) emission (e.g. Wilson 1966; Noyes et al. 1984; Soderblom et al. 1993), and radio emission from accelerated electrons (e.g.…”
Estimation of the XUV radiation onto close planets and their evaporation (2011, background): “Theτi parameter marks the typical change from saturation regime to an inverse proportionality betweenLX/Lbol and rotation period (e.g. Pizzolato et al., 2003).”
Stellar winds on the main-sequence - II. The evolution of rotation and winds (2015, methodology): “From the results of Pizzolato et al. (2003) and Reiners et al. (2014), we would expect that Ωsat, is 21 Ω and 17 Ω respectively.”
A CATALOG OF ROTATION AND ACTIVITY IN EARLY-M STARS (2012, background): “Observations of activity in 2 Reiners et al. solar-type stars show a direct connection between rotation and activity, the so-called rotation-activity relation (Noyes et al. 1984; Delfosse et al. 1998; Pizzolato et al. 2003).”
RADIUS-DEPENDENT ANGULAR MOMENTUM EVOLUTION IN LOW-MASS STARS. I (2011, background): “It is well established that chromospheric and coronal emission scale with rotation in the sense that, below a critical rotation velocity, emission is stronger with faster rotation, while above that velocity, activity is saturated (e.g., Pizzolato et al. 2003).”
ROTATION PERIODS OF 34,030 KEPLER MAIN-SEQUENCE STARS: THE FULL AUTOCORRELATION SAMPLE (2014, result): “Previous studies have suggested a typical increase in variability with rotation rate (e.g., Pizzolato et al. 2003; Hartman et al. 2011), although this was not seen by Basri et al. (2011).”
The Volume-limited A-Star (VAST) survey – I. Companions and the unexpected X-ray detection of B6–A7 stars (2011, result): “10 have unphysical high luminosity ratios, significantly higher than the observed luminosity ratios of late M-type stars (e.g. Pizzolato et al. 2003).”
Masses and Radii of Low-Mass Stars: Theory Versus Observations (2005, neutral): “As shown in the work by Pizzolato et al. (2003), any M-type star with a rotation period below 10 days will experience these phenomena at their peak (saturated activity).”
Habitable planets around the star Gliese 581 (2007, methodology): “This ratio is highest for the most active stars (i.e. fastest rotation period) and decreases monotonically with decreasing level of chromospheric activity (e.g., Stelzer & Neuhäuser, 2001; Pizzolato et al. 2003).”
THE EVOLUTION OF CATACLYSMIC VARIABLES AS REVEALED BY THEIR DONOR STARS (2011, neutral): “The specific dependence they aimed to reproduce was Lx,2 ∝ Ω2 at low Ω/Ω 2–12 and Lx,2 ∝ Ω0 for higher rotation speeds (Pizzolato et al. 2003).”
Stellar magnetism: empirical trends with age and rotation (2014, neutral): “0.1 (e.g., James et al. 2000; Pizzolato et al. 2003; Wright et al. 2011).”
TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS (2011, background): “For many stars the rotation rate also scales with age, chromospheric activity, and coronal X-ray emission (Skumanich 1972; Noyes et al. 1984; Pizzolato et al. 2003; Mamajek & Hillenbrand 2008).”