Both the viscous and MHD wind-driven disc evolution models fit the Lupus population demographics comparably, but require different ages and predict divergent evolutionary pathways for older regions.
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The Spitzer c2d Legacy Results: Star Formation Rates and Efficiencies; Evolution and Lifetimes
17 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
(Abridged) The c2d Spitzer Legacy project obtained images and photometry with both IRAC and MIPS instruments for five large, nearby molecular clouds. This paper combines information drawn from studies of individual clouds into a combined and updated statistical analysis of star formation rates and efficiencies, numbers and lifetimes for SED classes, and clustering properties. Current star formation efficiencies range from 3% to 6%. Taken together, the five clouds are producing about 260 solar masses of stars per Myr. The star formation surface density is more than an order of magnitude larger than would be predicted from the Kennicutt relation used in extragalactic studies. Measured against the dense gas probed by the maps of dust continuum emission, the efficiencies are much higher, and the current stock of dense cores would be exhausted in 1.8 Myr on average. The derived lifetime for the Class I phase is 0.44 to 0.54 Myr, considerably longer than some estimates. Similarly, the lifetime for the Class 0 SED class, 0.10 to 0.16 Myr, is longer than early estimates. The great majority (90%) of young stars lie within loose clusters with at least 35 members and a stellar density of 1 solar mass per cubic pc. Accretion at the sound speed from an isothermal sphere over the lifetime derived for the Class I phase could build a star of about 0.25 solar masses, given an efficiency of 0.3. Our data confirm and aggravate the "luminosity problem" for protostars. Our results strongly suggest that accretion is time variable, with prolonged periods of very low accretion. Based on a very simple model and this sample of sources, half the mass of a star would be accreted during only 7% of the Class I lifetime, as represented by the eight most luminous objects.
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Torsionally excited methanol (CH3OH vt>=1) lines in 12 massive clumps are compact, co-located with 24 micron emission, and scale with mid-IR luminosity, supporting their use as core-scale tracers of embedded protostars.
Serpens disk dust masses resemble Lupus and Taurus despite its high 2D stellar density, and the Ophiuchus and Corona Australis low-mass tension shifts to disks lacking Gaia identifications.
In simulated high-redshift galaxies, stellar mass is smooth while young-star light (Halpha, FUV, optical) is clumpy on 0.1-1 kpc scales, with clumpiness tracking bursty star formation and feedback strength.
A potential new outflow cavity at a previously unseen position angle is detected in redshifted 13CO and C18O around the proto-brown-dwarf candidate IRAM04191+1522.
Five protostars from 0.16 to 10,000 solar luminosities show nested, onion-like H2 outflows, with higher-excitation gas more collimated and faster, consistent with MHD disk wind launching.
Observations and a pressure-balance model of HOPS 198 link a 2.9x difference in inferred core pressure to the 80 versus 30 degree asymmetry in outflow opening angle, supporting a density-driven evolution of outflow widths.
Cloud-fed ideal-MHD zoom-in simulations of nine young stars show discs are replenished on ~10,000-year timescales via surface-layer accretion and can be truncated by massive streamers.
Disks around young stars in binary and higher-order multiple systems are preferentially aligned out to 6000 AU, implying turbulent fragmentation alone cannot explain how most multiples form.
In Orion, turbulence dissipates in high-shear regions near dense fibers, so the transition to coherence occurs at the fiber level before cores form.
Turbulence strength strongly reshapes the stellar mass distribution: the lowest-Mach-number cloud in these simulations forms a bimodal IMF, while higher-Mach clouds resemble observed IMFs.
Two catalogued X-ray-detected Be stars are reclassified as a classical Be star rotating in 0.355 days and an accreting, UX Ori-type Herbig Be star, both with steady, moderately hard Chandra X-ray emission of plausible but unproven magnetic origin.
Disks form in all six simulated magnetized turbulent cores, with ideal and non-ideal MHD producing similar disk properties; ideal-MHD disks sit in smaller, shorter-lived rotating envelopes.
A next-generation millimeter interferometer with tenfold sensitivity gains would detect embedded protoplanets, outflow tracers, and two-Earth-mass disks whose presence can distinguish star-like from planet-like formation of brown dwarfs.
SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.
This review consolidates current knowledge on how stellar multiplicity shapes protoplanetary disc structure, dust evolution, and planet formation outcomes.
citing papers explorer
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DEMOS. II. What the full Lupus demographics truly tell us about protoplanetary disc evolution
Both the viscous and MHD wind-driven disc evolution models fit the Lupus population demographics comparably, but require different ages and predict divergent evolutionary pathways for older regions.
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Torsionally excited methanol in massive young stellar objects: The role of the mid-IR radiation field
Torsionally excited methanol (CH3OH vt>=1) lines in 12 massive clumps are compact, co-located with 24 micron emission, and scale with mid-IR luminosity, supporting their use as core-scale tracers of embedded protostars.
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Disk survey in the Serpens star-forming region: Environmental effects in nearby star-forming regions
Serpens disk dust masses resemble Lupus and Taurus despite its high 2D stellar density, and the Ophiuchus and Corona Australis low-mass tension shifts to disks lacking Gaia identifications.
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The THESAN-ZOOM project: clumpiness of high-redshift galaxies and its connection to bursty star formation
In simulated high-redshift galaxies, stellar mass is smooth while young-star light (Halpha, FUV, optical) is clumpy on 0.1-1 kpc scales, with clumpiness tracking bursty star formation and feedback strength.
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Complex morphology and kinematics at the heart of the very low luminosity object IRAM 04191+1522
A potential new outflow cavity at a previously unseen position angle is detected in redshifted 13CO and C18O around the proto-brown-dwarf candidate IRAM04191+1522.
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IPA: Morphology and Kinematics of Molecular Hydrogen Winds in Five Young Protostars across the Mass Spectrum Observed with JWST
Five protostars from 0.16 to 10,000 solar luminosities show nested, onion-like H2 outflows, with higher-excitation gas more collimated and faster, consistent with MHD disk wind launching.
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Asymmetry in the protostellar system HOPS 198: Evidence for the evolution of outflow opening angle driven by density of the surrounding core
Observations and a pressure-balance model of HOPS 198 link a 2.9x difference in inferred core pressure to the 80 versus 30 degree asymmetry in outflow opening angle, supporting a density-driven evolution of outflow widths.
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Accretion across scales: streamers, surface-layer transport, and rapid replenishment in young protoplanetary discs
Cloud-fed ideal-MHD zoom-in simulations of nine young stars show discs are replenished on ~10,000-year timescales via surface-layer accretion and can be truncated by massive streamers.
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Preferential alignment of Class 0, Class I protostellar disks in multiple systems across nine nearby molecular clouds
Disks around young stars in binary and higher-order multiple systems are preferentially aligned out to 6000 AU, implying turbulent fragmentation alone cannot explain how most multiples form.
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Emergence of high-mass stars in complex fiber networks (EMERGE) VI. Turbulence dissipation and the formation of dense fibers
In Orion, turbulence dissipates in high-shear regions near dense fibers, so the transition to coherence occurs at the fiber level before cores form.
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The impact of the turbulent Mach number on star formation and the initial mass function
Turbulence strength strongly reshapes the stellar mass distribution: the lowest-Mach-number cloud in these simulations forms a bimodal IMF, while higher-Mach clouds resemble observed IMFs.
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A comprehensive multi-wavelength study of two X-ray emitting Be stars
Two catalogued X-ray-detected Be stars are reclassified as a classical Be star rotating in 0.355 days and an accreting, UX Ori-type Herbig Be star, both with steady, moderately hard Chandra X-ray emission of plausible but unproven magnetic origin.
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Non-ideal MHD and protostellar feedback effects on disc formation and evolution in numerical simulations of star cluster formation
Disks form in all six simulated magnetized turbulent cores, with ideal and non-ideal MHD producing similar disk properties; ideal-MHD disks sit in smaller, shorter-lived rotating envelopes.
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Bridging the gap between stars and planets
A next-generation millimeter interferometer with tenfold sensitivity gains would detect embedded protoplanets, outflow tracers, and two-Earth-mass disks whose presence can distinguish star-like from planet-like formation of brown dwarfs.
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Early phases of star formation with SKAO: synchrotron emission from dense starless cores in molecular clouds
SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.
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Circumstellar and circumbinary discs in multiple stellar systems
This review consolidates current knowledge on how stellar multiplicity shapes protoplanetary disc structure, dust evolution, and planet formation outcomes.
- Grain alignment and dust evolution physics with polarisation (GRADE-POL). II. On the physical basis of Serkowski and super-Serkowski polarisation spectra