Epilogue

Clarke, Katherine

doi:10.1093/acprof:oso/9780199291083.003.0007

Cited by 6 publications

(9 citation statements)

References 87 publications

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“…According to Clarke & Pringle (2006) and Tilling et al (2008), the upper bound of the Lacc-L * correlation (Lacc ∼ L * ) is the consequence of sample selection effects; the luminosity of most stars above that limit is dominated by accretion and these objects are in a younger, embedded phase without an optically visible photosphere. The lower bound (Lacc ∼ 0.01L * , mainly for objects with L * > L⊙) is limited by accretion detection thresholds (symbols with vertical bars in Fig.…”

Section: The Lacc -L * Correlationmentioning

confidence: 99%

“…The Lacc-L * correlation extends over ∼ 10 orders of magnitude in Lacc, and ∼ 7 orders of magnitude in L * , covering all optically visible young stars from the substellar to the HAeBe regime (see e.g. Natta et al 2006;Clarke & Pringle 2006;Tilling et al 2008;Mendigutía et al 2011;Fairlamb et al 2015, and references therein). Based on a statistical analysis, Mendigutía et al (2011) tentatively suggested that the correlation between the accretion luminosity and the luminosity of several emission lines in HAeBe stars could be driven by the common dependence of both luminosities on the stellar luminosity.…”

mentioning

confidence: 99%

“…Its counterpart, the relationship between mass accretion rate and stellar mass, can be derived from the Lacc-L * correlation using PMS tracks (see e.g Clarke & Pringle 2006)…”

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confidence: 99%

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On the origin of the correlations between the accretion luminosity and emission line luminosities in pre-main-sequence stars

Mendigutía

Oudmaijer

Rigliaco

et al. 2015

Mon. Not. R. Astron. Soc.

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Correlations between the accretion luminosity and emission line luminosities (L acc and L line ) of pre-main sequence (PMS) stars have been published for many different spectral lines, which are used to estimate accretion rates. Despite the origin of those correlations is unknown, this could be attributed to direct or indirect physical relations between the emission line formation and the accretion mechanism. This work shows that all (near-UV/optical/near-IR) L acc -L line correlations are the result of the fact that the accretion luminosity and the stellar luminosity (L * ) are correlated, and are not necessarily related with the physical origin of the line. Synthetic and observational data are used to illustrate how the L acc -L line correlations depend on the L acc -L * relationship. We conclude that because PMS stars show the L acc -L * correlation immediately implies that L acc also correlates with the luminosity of all emission lines, for which the L acc -L line correlations alone do not prove any physical connection with accretion but can only be used with practical purposes to roughly estimate accretion rates. When looking for correlations with possible physical meaning, we suggest that L acc /L * and L line /L * should be used instead of L acc and L line . Finally, the finding that L acc has a steeper dependence on L * for T-Tauri stars than for intermediatemass Herbig Ae/Be stars is also discussed. That is explained from the magnetospheric accretion scenario and the different photospheric properties in the near-UV.

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Section: The Lacc -L * Correlationmentioning

confidence: 99%

mentioning

confidence: 99%

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On the origin of the correlations between the accretion luminosity and emission line luminosities in pre-main-sequence stars

Mendigutía

Oudmaijer

Rigliaco

et al. 2015

Mon. Not. R. Astron. Soc.

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“…The columns of material accreting onto a young star also emit hydrogen emission lines that are significantly stronger and broader than those from stellar chromospheres, offering an additional tracer of accretion. Because Hα is more easily observed in brown dwarfs than UV emission, line profiles of Hα provided the first evidence of accretion for young low-mass objects gested that this apparent correlation may be largely due to selection effects (Clarke & Pringle 2006). If a dependence on stellar mass is present, its origin is unclear (Hartmann et al 2006, Vorobyov & Basu 2009).…”

Section: Circumstellar Disksmentioning

confidence: 99%

The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs

Luhman

2012

Annu. Rev. Astron. Astrophys.

207

158

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The discovery of large numbers of young low-mass stars and brown dwarfs over the last decade has made it possible to investigate star formation and early evolution in a previously unexplored mass regime. In this review, we begin by describing surveys for low-mass members of nearby associations, open clusters, star-forming regions and the methods used to characterize their stellar properties. We then use observations of these populations to test theories of star formation and evolution at low masses. For comparison to the formation models, we consider the initial mass function, stellar multiplicity, circumstellar disks, protostellar characteristics, and kinematic and spatial distributions at birth for low-mass stars and brown dwarfs. To test the evolutionary models, we focus on measurements of dynamical masses and empirical Hertzsprung-Russell diagrams for young brown dwarfs and planetary companions.

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“…However, the detection limits and the difficulty of measuring very smallṀ do not allow us to rule out detection/selection thresholds as responsible for this trend (see e.g. Clarke & Pringle 2006). Moreover, the spread of theṀ data exceeds 2 dex at any given age.…”

Section: Introductionmentioning

confidence: 98%

Photometric determination of the mass accretion rates of pre-mainsequence stars - III. Results in the Large Magellanic Cloud

Spezzi¹,

Marchi²,

Panagia³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2012 RAS © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.We present a multiwavelength study of three star-forming regions, spanning the age range 1-14Myr, located between the 30 Doradus complex and supernova SN 1987A in the Large Magellanic Cloud (LMC). We reliably identify about 1000 pre-main-sequence (PMS) star candidates actively undergoing mass accretion and estimate their stellar properties and mass accretion rate (M). Our measurements represent the largest M data set of low-metallicity stars presented so far. As such, they offer a unique opportunity to study on a statistical basis the mass accretion process in the LMC and, more in general, the evolution of the mass accretion process around low-metallicity stars. We find that the typical M of PMS stars in the LMC is higher than for galactic PMS stars of the same mass, independently of their age. Taking into account the caveats of isochronal age and M estimates, the difference in M between the LMC and our Galaxy appears to be about an order of magnitude. We review the main mechanisms of disc dispersal and find indications that typically higher M are to be expected in low-metallicity environments. However, many issues of this scenario need to be clarified by future observations and modelling. We also find that, in the mass range 1-2M ⊙, M of PMS stars in the LMC increases with stellar mass as M ∝ M * b, with b≈ 1, i.e. slower than the second power law found for galactic PMS stars in the same mass regim

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Epilogue

Cited by 6 publications

References 87 publications

On the origin of the correlations between the accretion luminosity and emission line luminosities in pre-main-sequence stars

On the origin of the correlations between the accretion luminosity and emission line luminosities in pre-main-sequence stars

The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs

Photometric determination of the mass accretion rates of pre-mainsequence stars - III. Results in the Large Magellanic Cloud

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