The "rotation-activity connection": Its extension to photospheric activity diagnostics

Messina, S.; Rodono, M.; Guinan, E. F.

doi:10.1051/0004-6361:20000201

Cited by 74 publications

(92 citation statements)

References 53 publications

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“…As discussed in Paper I, there is some marginal (yet) evidence of some other age-dependent quantity, in addition to mass and rotation, that controls the level of (photospheric at least) activity and makes older stars less active than younger stars (see also Messina et al 2010). A similar suspect has already been raised by Messina et al (2001), who found evidence that, for a fixed mass and rotation period, the level of starspot activity increases (or alternatively the gross surface distribution of spots changes) from the zero-age main sequence up to the Pleiades age (∼120 Myr) and then it decreases with age. With the data of M 11 G stars in hand, we can state that up to the M 11 age the level of activity remains at highest levels.…”

Section: Photospheric Activitymentioning

confidence: 68%

“…This is consistent with the expected dependence on rotation rate of the efficiency of magnetic field generation and intensification by an αΩ dynamo. The solid line represents the fit to the upper envelope of the light curve amplitude distribution of slowly rotating Pleiades G stars (110 Myr) taken from Messina et al (2001Messina et al ( , 2003. With the data at our disposal, we do not see any significant difference between the 110-Myr and the 230-Myr distribution upper envelopes.…”

Section: Photospheric Activitymentioning

confidence: 81%

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RACE-OC project: rotation and variability in the open cluster M 11 (NGC 6705)

Messina

Parihar

Koo

et al. 2010

A&A

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Context. Rotation and magnetic activity are intimately linked in main-sequence stars of G or later spectral types. The presence and level of magnetic activity depend on stellar rotation, and rotation itself is strongly influenced by the strength and topology of the magnetic fields. Open clusters represent especially useful targets for investigating the connection among rotation, activity, and age. Over time, stellar activity and rotation evolve, providing us with a promising diagnostic tool to determine the age of the field stars.Aims. The open cluster M11 has been studied as a part of the RACE-OC project (Rotation and ACtivity Evolution in Open Clusters), which aims to explore the evolution of rotation and magnetic activity in the late-type members of open clusters with different ages. Methods. Photometric observations of the open cluster M 11 were carried out in June 2004 using the LOAO 1 m telescope. The rotation periods of the cluster members were determined by Fourier analysis of photometric data time series. We investigated the relations between the surface activity, characterized by the light curve amplitude, and rotation. Results. We have discovered a total of 75 periodic variables in the M 11 FoV, of which 38 are candidate cluster members. Specifically, among cluster members we discovered 6 early-type periodic variables, 2 eclipsing binaries, and 30 bona-fide single periodic late-type variables. Considering the rotation periods of 16 G-type members of the almost coeval 200-Myr M 34 cluster, we could determine the rotation period distribution from a more numerous sample of 46 single G stars at an age of about 200-230 Myr and determine a median rotation period of P = 4.8 d. Conclusions. A comparison with the younger M 35 cluster (∼150 Myr) and with the older M37 cluster (∼550 Myr) shows that G stars rotate more slowly than younger M 35 stars and more rapidly than older M 37 stars. The measured variation in the median rotation period is consistent with the scenario of rotational braking of main-sequence spotted stars as they age. Finally, G-type M11 members have a level of photospheric magnetic activity, as measured by light curve amplitude, comparable to what is observed in the younger 110-Myr Pleiades stars of similar mass and rotation.

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Section: Photospheric Activitymentioning

confidence: 68%

Section: Photospheric Activitymentioning

confidence: 81%

RACE-OC project: rotation and variability in the open cluster M 11 (NGC 6705)

Messina

Parihar

Koo

et al. 2010

A&A

Self Cite

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“…The amplitude of the light curve provides a lower limit on the amount of magnetic fields asymmetrically distributed along the stellar longitude, which is in turn proportional to the total magnetic field filling factor. As shown by Messina et al (2001, the upper bound of the light curve amplitude distribution is observed to decrease with increasing rotation period, when the dynamo becomes less efficient. In Fig.…”

Section: Rotation-photospheric Activity Connectionmentioning

confidence: 89%

RACE-OC project: Rotation and variability of young stellar associations within 100 pc

Messina

Desidera²,

Turatto

et al. 2010

A&A

Self Cite

121

161

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Context. Angular momentum and its interplay with magnetic fields represent a promising tool to probe the stellar internal structure and evolution of low-mass stars Aims. Our goal is to determine the rotational and magnetic-related activity properties of stars at different stages of evolution. For this reason, we have focussed our attention primarily on members of clusters and young stellar associations of known ages. In this study, our targets are 6 young loose stellar associations within 100 pc and ages in the range 8-70 Myr: TW Hydrae (∼8 Myr), β Pictoris (∼10 Myr), Tucana/Horologium, Columba, Carina (∼30 Myr), and AB Doradus (∼70 Myr). Additional data on α Persei and the Pleiades from the literature is also considered. Methods. Rotational periods of stars showing rotational modulation due to photospheric magnetic activity (i.e. starspots) have been determined applying the Lomb-Scargle periodogram technique to photometric time-series obtained by the All Sky Automated Survey (ASAS). The magnetic activity level has been derived from the amplitude of the V lightcurves. The statistical significance of the rotational evolution at different ages has been inferred applying a twosided Kolmogorov-Smirnov test to subsequent age-bins. Results. We detected the rotational modulation and measured the rotation periods of 93 stars for the first time, and confirmed the periods of 41 stars already known from the literature. For further 10 stars we revised the period determinations by other authors. The sample was augmented with periods of 21 additional stars retrieved from the literature. In this way, for the first time we were able to determine largest set of rotation periods at ages of ∼8, ∼10 and ∼30 Myr, as well as increase by 150% the number of known periodic members of AB Dor. Conclusions. The analysis of the rotation periods in young stellar associations, supplemented by Orion Nebula Cluster (ONC) and NGC 2264 data from the literature, has allowed us to find that in the 0.6 -1.2 M⊙ range the most significant variations of the rotation period distribution are the spin-up between 9 and 30 Myr and the spin-down between 70 and 110 Myr. Variations between 30 and 70 Myr are rather doubtful, despite the median period indicates a significant spin-up. The photospheric activity level is found to be correlated to rotation at ages greater than ∼70 Myr and to show some additional age dependence beside that related to rotation and mass.

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“…Column 14 contains important notes: spectroscopic binaries radial velocities standards, and stars in chromospherically active binary systems are identified in this column. Tables 9 to 13 Baliunas et al (1996); (3) Duncan et al (1991) calculated using equations in Noyes et al (1984); (4) Gray et al (2003); (5) Gray et al (2006); (6) Hall et al (2007); (7) Henry et al (1996); (8) Jenkins et al (2006); (9) Saffe et al (2005); (10) Wright et al (2004); (11) estimated form ROSAT-data using equation A1 in Mamajek & Hillenbrand (2008); (12) Noyes et al (1984); (13) Saar & Osten (1997); (14) Messina et al (2001).…”

Section: Appendix A: Tablesmentioning

confidence: 99%

A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups

Maldonado¹,

Martínez-Arnáiz

Eiroa³

et al. 2010

A&A

109

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Context. Nearby late-type stars are excellent targets for seeking young objects in stellar associations and moving groups. The origin of these structures is still misunderstood, and lists of moving group members often change with time and also from author to author. Most members of these groups have been identified by means of kinematic criteria, leading to an important contamination of previous lists by old field stars. Aims. We attempt to identify unambiguous moving group members among a sample of nearby-late type stars by studying their kinematics, lithium abundance, chromospheric activity, and other age-related properties. Methods. High-resolution echelle spectra (R ∼ 57 000) of a sample of nearby late-type stars are used to derive accurate radial velocities that are combined with the precise Hipparcos parallaxes and proper motions to compute galactic-spatial velocity components. Stars are classified as possible members of the classical moving groups according to their kinematics. The spectra are also used to study several age-related properties for young late-type stars, i.e., the equivalent width of the lithium Li i 6707.8 Å line or the R HK index. Additional information like X-ray fluxes from the ROSAT All-Sky Survey or the presence of debris discs is also taken into account. The different age estimators are compared and the moving group membership of the kinematically selected candidates are discussed. Results. From a total list of 405 nearby stars, 102 have been classified as moving group candidates according to their kinematics. i.e., only ∼25.2% of the sample. The number reduces when age estimates are considered, and only 26 moving group candidates (25.5% of the 102 candidates) have ages in agreement with the star having the same age as an MG member.

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The "rotation-activity connection": Its extension to photospheric activity diagnostics

Cited by 74 publications

References 53 publications

RACE-OC project: rotation and variability in the open cluster M 11 (NGC 6705)

RACE-OC project: rotation and variability in the open cluster M 11 (NGC 6705)

RACE-OC project: Rotation and variability of young stellar associations within 100 pc

A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups

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