STELLAR ROTATION IN M35: MASS–PERIOD RELATIONS, SPIN-DOWN RATES, AND GYROCHRONOLOGY

By S. Meibom, R. Mathieu, Keivan G. Stassun. 2008

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We present the results of a five month photometric time-series survey for stellar rotation over a 40′ × 40′ field centered on the 150 Myr open cluster M35. We report rotation periods for 441 stars within this field and determine their cluster membership and binarity based on a decade-long radial velocity survey, proper-motion measurements, and multiband photometric observations. We find that 310 of the stars with measured rotation periods are late-type members of M35. The distribution of rotation periods for cluster members span more than 2 orders of magnitude from ∼0.1 to 15 days, not constrained by the sampling frequency and the timespan of the survey. With an age between the zero-age main sequence and the Hyades, and with ∼6 times more rotation periods than measured in the Pleiades, M35 permit detailed studies of early rotational evolution of late-type stars. Nearly 80% of the 310 rotators lie on two distinct sequences in the color–period plane, and define clear relations between stellar rotation period and color (mass). The M35 color–period diagram enables us to determine timescales for the transition between the two rotational states, of ∼60 Myr and ∼140 Myr for G and K dwarfs, respectively. These timescales are inversely related to the mass of the convective envelope, and offer constraints on the rates of internal and external angular momentum transport and of the evolution of stellar dynamos. A comparison to the Hyades, confirm the Skumanich spin-down dependence for G dwarfs on one rotational state, but suggest that K dwarfs spin down more slowly. The locations of the rotational sequences in the M35 color–period diagram support the use of rotational isochrones to determine ages for coeval stellar populations. We use such gyrochronology to determine “gyro-ages” for M35 from 134 Myr to 161 Myr. We use the M35 data to evaluate new color dependences for the rotational isochrones.

Subfields: Astronomy and Astrophysics, Education, Instrumentation

View Paper: https://www.semanticscholar.org/paper/952a2c810824be2683412ef506bd793ba3d3206d

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Citations in the corpus

Improved angular momentum evolution model for solar-like stars (2013, methodology): “We used the Siess et al. (2000) 130 Myr isochrones together with the (B − V )0 measurements from Meibom et al. (2009) to estimate the stellar masses.”
Rotation and magnetism of Kepler pulsating solar-like stars : Towards asteroseismically calibrated age-rotation relations (2014, methodology): “Several calibrations are reported in the literature (Pace & Pasquini 2004; Barnes 2007; Mamajek & Hillenbrand 2008; Meibom et al. 2009, 2011a), but they consistently struggle to find a calibration set at old ages and long rotation periods.”
Stellar winds on the main-sequence - II. The evolution of rotation and winds (2015, methodology): “…recent derivation of the dependence of wind torque on mass loss rate (Matt et al. 2012), and a recent series of excellent observational campaigns measuring rotation in young stellar clusters (e.g. Irwin et al. 2007; Hartman et al. 2009; Irwin et al. 2009; Meibom et al. 2009; Hartman et al. 2010).”
THE KEPLER CLUSTER STUDY: STELLAR ROTATION IN NGC 6811 (2011, background): “For stars in young (∼100Myr) clusters the relationship between P and M is not unique, and the surface splits into two (fast and slow) branches (e.g. Barnes 2003; Hartman et al. 2009, 2010; Meibom et al. 2009, 2011; Irwin et al. 2009; James et al. 2010).”
ROTATION PERIODS OF 34,030 KEPLER MAIN-SEQUENCE STARS: THE FULL AUTOCORRELATION SAMPLE (2014, methodology): “A comparison to empirical gyrochronology models (Barnes 2007; Mamajek & Hillenbrand 2008; Meibom et al. 2009) shows the upper envelope of points is broadly consistent with an age of 4.5Gyrs, but that the models appear to under-predict the stellar ages, with a significant proportion falling below…”
THE MASS-DEPENDENCE OF ANGULAR MOMENTUM EVOLUTION IN SUN-LIKE STARS (2014, background): “…of stellar spin rate in time (e.g., MacGregor & Brenner 1991; Denissenkov et al. 2010; Scholz et al. 2011; Reiners & Mohanty 2012; Gallet & Bouvier 2013; van Saders & Pinsonneault 2013; Brown 2014); and gyrochronology relations (Barnes 2003, 2010; Mamajek & Hillenbrand 2008; Meibom et al. 2009).”
Measuring the rotation period distribution of field M dwarfs with Kepler (2013, background): “Notable, more recent additions to the literature on rotation of early main-sequence lowmass stars include studies of M37 (Meibom et al. 2009) and Coma Berenices (Collier Cameron et al. 2009).”
A PHOTOMETRIC VARIABILITY SURVEY OF FIELD K AND M DWARF STARS WITH HATNet (2009, methodology): “These include M35 (∼180 Myr; Meibom et al. 2009), three clusters observed by the MONITOR project, including M50 (∼130 Myr; Irwin et al. 2009a), NGC 2516 (∼150 Myr; Irwin et al. 2007), and M34 (∼200 Myr; Irwin et al. 2006), M37 (∼550 Myr; Hartman et al. 2009), Coma Berenices (∼600 Myr; Collier Camero”
THE STELLAR-ACTIVITY–ROTATION RELATIONSHIP AND THE EVOLUTION OF STELLAR DYNAMOS (2011, background): “It is worth noting that, at the ages considered here, differences between the gyrochronological parameters of Barnes (2003b), Mamajek & Hillenbrand (2008), and Meibom et al. (2009) are too small to be discernible in this figure.”
Rotation, differential rotation, and gyrochronology of active Kepler stars (2015, methodology): “…periods P and period variations ∆P for two-thirds of the sample, we calculate stellar ages t along with their uncertainties ∆t using different gyrochronology relations (Barnes 2007; Mamajek & Hillenbrand 2008; Meibom et al. 2009), hereafter abbre- viated as B07, MH08, and MMS09, respectively.”
DIRECT IMAGING OF A COLD JOVIAN EXOPLANET IN ORBIT AROUND THE SUN-LIKE STAR GJ 504 (2013, methodology): “Previously Imaged Planet Candidates Some of the previously imaged exoplanets were discovered around young (10–50 Myr), relatively massive stars like HR 8799 (1.5 M⊙; 20–50 Myr; Marois et al. 2008, 2010) and β Pictoris (1.75 M⊙; 10–20 Myr; Lagrange et al. 2010), with masses estimated at 5–9 MJup, ass”