Star Formation in the Orion Nebula Cluster

Palla, F.; Stahler, Steven W.

doi:10.1086/307928

Cited by 518 publications

(866 citation statements)

References 75 publications

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“…HR-diagram with PMS evolutionary tracks (solid lines labeled by the corresponding masses in M ) from Siess et al (1997) for M ≤ 7 M and from Bernasconi & Maeder (1996) for M ≥ 9 M . The upper dashed-dotted line is the stellar birthline according to Palla & Stahler (1999), the lower dashed-dotted line shows the 1 Myr isochrone. The positions of the primary stars are shown by the squares.…”

Section: Spectroscopic Results For the θ 1 Ori C Systemmentioning

confidence: 99%

“…These bands can now be compared to PMS evolutionary models, in order to estimate stellar masses. Given the uncertainties in the colors derived from the flux-ratios, it seems useful to take two further constraints into account: we expect the position of the YSOs in the HR-diagram to be below the birthline (see Palla & Stahler 1999) and above the 1 Myr isochrone 5 .…”

Section: Near-infrared Magnitudes Of the Components And Stellar Mass mentioning

confidence: 99%

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Orbital motion of the massive multiple stars in the Orion Trapezium

Schertl

Balega

Preibisch

et al. 2003

A&A

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Abstract. We present bispectrum speckle interferometry of the multiple Orion Trapezium stars θ 1 Ori A, θ 1 Ori B, and θ 1 Ori C obtained with the SAO 6 m telescope in Russia over a period of 5.5 years (epochs 1995-2001). Our diffraction-limited images have a resolution λ/D of 42 mas (J-band), 57 mas (H-band) and 76 mas (K-band). We clearly detect motion of the companions relative to their primary stars in the systems θ 1 Ori A1-2 (mean separation ρ ∼ 220 mas, change in position angle ∆PA = 6 • ), θ 1 Ori B2-3 (ρ ∼ 205 mas, ∆PA = 8 • ), and θ 1 Ori C1-2 (ρ ∼ 37 mas, ∆PA = 18 • ). In our K-band image of θ 1 Ori B we resolve a fourth visual component, confirming its discovery by Simon et al. (1999). We determine the J, H, and K magnitudes of the system components and estimate the stellar masses of the companions in the HR-diagram. The companions θ 1 Ori C2 and θ 1 Ori B2 show clear evidence of near-infrared excess in the color-color diagram. The companions θ 1 Ori A2 and θ 1 Ori B3 show much stronger extinction than their primary stars, providing evidence of the presence of circumstellar material around the companions.

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Section: Spectroscopic Results For the θ 1 Ori C Systemmentioning

confidence: 99%

Section: Near-infrared Magnitudes Of the Components And Stellar Mass mentioning

confidence: 99%

Orbital motion of the massive multiple stars in the Orion Trapezium

Schertl

Balega

Preibisch

et al. 2003

A&A

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“…He presumed that lowmass star formation occurred prior to the formation of highmass stars, and that star formation within a cluster could be prolonged for up to~10 8 years. Palla & Stahler (1999, 2000 suggested a revised version of the sequential star formation speculated by Herbig (1962) using their own PMS evolutionary models. According to their argument, star formation started at an early epoch (about 10 Myr ago), and then the star formation rate accelerated in the present epoch (1-2 Myr ago).…”

Section: Introductionmentioning

confidence: 99%

A Constraint on the Formation Timescale of the Young Open Cluster NGC 2264: Lithium Abundance of Pre-Main Sequence Stars

Lim

Sung

Kim

et al. 2016

ApJ

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The timescale of cluster formation is an essential parameter in order to understand the formation process of star clusters. Pre-main sequence (PMS) stars in nearby young open clusters reveal a large spread in brightness. If the spread were considered to be a result of a real spread in age, the corresponding cluster formation timescale would be about 5-20 Myr. Hence it could be interpreted that star formation in an open cluster is prolonged for up to a few tens of Myr. However, difficulties in reddening correction, observational errors, and systematic uncertainties introduced by imperfect evolutionary models for PMS stars can result in an artificial age spread. Alternatively, we can utilize Li abundance as a relative age indicator of PMS star to determine the cluster formation timescale. The optical spectra of 134 PMS stars in NGC 2264 have been obtained with MMT/Hectochelle. The equivalent widths have been measured for 86 PMS stars with a detectable Li line (). Li abundance under the condition of local thermodynamic equilibrium (LTE) was derived using the conventional curve of growth method. After correction for non-LTE effects, we find that the initial Li abundance of NGC 2264 is. From the distribution of the Li abundances, the underlying age spread of the visible PMS stars is estimated to be about 3-4 Myr and this, together with the presence of embedded populations in NGC 2264, suggests that the cluster formed on a timescale shorter than 5 Myr.

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“…Recently, considerable advances have been made in our understanding of PMS evolution (Palla & Stahler 1999;Siess, Dufour, & Forestini 2000;Baraffe et al 2002;Tognelli, Prada Moroni, & Degl'Innocenti 2011). However, differences in the evolutionary tracks remain due to the different treatment of convection, different opacities and differences in the zero-point of the calculated ages.…”

Section: Introductionmentioning

confidence: 99%

Keplerobservations of A–F pre-main-sequence stars in Upper Scorpius: discovery of six new δ Scuti and one γ Doradus stars

Ripepi¹,

Balona²,

Catanzaro³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present light curves and periodograms for 27 stars in the young Upper Scorpius association (age=11 ± 1 Myr) obtained with the Kepler spacecraft. This association is only the second stellar grouping to host several pulsating pre-main sequence (PMS) stars which have been observed from space.From an analysis of the periodograms, we identify six δ Scuti variables and one γ Doradus star. These are most likely PMS stars or else very close to the zero-age main sequence. Four of the δ Scuti variables were observed in short-cadence mode, which allows us to resolve the entire frequency spectrum. For these four stars, we are able to infer some qualitative information concerning their ages. For the remaining two δ Scuti stars, only long-cadence data are available, which means that some of the frequencies are likely to be aliases. One of the stars appears to be a rotational variable in a hierarchical triple system. This is a particularly important object, as it allows the possibility of an accurate mass determination when radial velocity observations become available. We also report on new high-resolution echelle spectra obtained for some of the stars of our sample.

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Star Formation in the Orion Nebula Cluster

Cited by 518 publications

References 75 publications

Orbital motion of the massive multiple stars in the Orion Trapezium

Orbital motion of the massive multiple stars in the Orion Trapezium

A Constraint on the Formation Timescale of the Young Open Cluster NGC 2264: Lithium Abundance of Pre-Main Sequence Stars

Keplerobservations of A–F pre-main-sequence stars in Upper Scorpius: discovery of six new δ Scuti and one γ Doradus stars

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