3,681 research outputs found
Stellar evolution before the ZAMS
Young stars on their way to the ZAMS evolve in significantly different ways
depending on mass. While the theoretical and observational properties of low-
and intermediate-mass stars are rather well understood and/or empirically
tested, the situation for massive stars (>10-15 Msun) is, to say the least,
still elusive. On theoretical grounds, the PMS evolution of these objects
should be extremely short, or nonexistent at all. Observationally, despite a
great deal of effort, the simple (or bold) predictions of simplified models of
massive star formation/evolution have proved more difficult to be checked.
After a brief review of the theoretical expectations, I will highlight some
critical test on young stars of various masses.Comment: To appear in Massive Star Birth: A Crossroads fro Astrophysics, eds.
R. Cesaroni et al. (CUP
The Pre--Main-Sequence of A-type stars
Young A-type stars in the pre--main-sequence (PMS) evolutionary phase are
particularly interesting objects since they cover the mass range (1.5-4 solar
ma sses) which is most sensitive to the internal conditions inherited during
the protostellar phase. In particular, they undergo a process of thermal
relaxation from which they emerge as fully radiative objects contracting
towards the main sequence. A-type stars also show intense surface activity
(including winds, accretion, pulsations) whose origin is still not completely
understood, and infrared excesses related to the presence of circumstellar
disks and envelopes. Disks display significant evolution in the dust
properties, likely signalling the occurrence of protoplanetary growth. Finally,
A-type stars are generally found in multiple systems and small aggregates of
lower mass companions.Comment: 10 pages, 6 postscript figures, Proceedings of IAU Symp 224 (Poprad
July 2004
Post-T Tauri stars: a false problem
We consider the problem of the apparent lack of old T Tauri stars in low-mass
star forming regions in the framework of the standard model of low-mass star
formation. We argue that the similarity between molecular cloud lifetime and
ambipolar diffusion timescale implies that star formation does not take place
instantaneously, nor at a constant rate. We conclude that the probability of
finding a large population of old stars in a star forming region is
intrinsically very small and that the post-T Tauri problem is by and large not
existent.Comment: 6 pages (LaTeX), no Figures to be published in The Astrophysical
Journal Letter
Non-thermal photons and H2 formation in the early Universe
The cosmological recombination of H and He at z \sim 1000 and the formation
of H2 during the dark ages produce a non-thermal photon excess in the Wien tail
of the cosmic microwave background (CMB) blackbody spectrum. Here we compute
the effect of these photons on the H- photodetachment and H2+ photodissociation
processes. We discuss the implications for the chemical evolution of the
Universe in the post-recombination epoch, emphasizing how important a detailed
account of the full vibrational manifold of H2 and H2+ in the chemical network
is. We find that the final abundances of H2, H2+, H3+ and HD are significantly
smaller than in previous calculations that neglected the effect of non-thermal
photons. The suppression is mainly caused by extra hydrogen recombination
photons and could affect the formation rate of first stars. We provide simple
analytical approximations for the relevant rate coefficients and briefly
discuss the additional effect of dark matter annihilation on the considered
reaction rates.Comment: 10 pages, 12 figures, 1 table; accepted for publication in MNRA
Massive black hole factories: Supermassive and quasi-star formation in primordial halos
Supermassive stars and quasi-stars (massive stars with a central black hole)
are both considered as potential progenitors for the formation of supermassive
black holes. They are expected to form from rapidly accreting protostars in
massive primordial halos. We explore how long rapidly accreting protostars
remain on the Hayashi track, implying large protostellar radii and weak
accretion luminosity feedback. We assess the potential role of energy
production in the nuclear core, and determine what regulates the evolution of
such protostars into quasi-stars or supermassive stars. We follow the
contraction of characteristic mass scales in rapidly accreting protostars, and
infer the timescales for them to reach nuclear densities. We compare the
characteristic timescales for nuclear burning with those for which the extended
protostellar envelope can be maintained. We find that the extended envelope can
be maintained up to protostellar masses of 3.6x10^8 \dot{m}^3 solar, where
\dot{m} denotes the accretion rate in solar masses per year. We expect the
nuclear core to exhaust its hydrogen content in 7x10^6 yrs. If accretion rates
\dot{m}>>0.14 can still be maintained at this point, a black hole may form
within the accreting envelope, leading to a quasi-star. Alternatively, the
accreting object will gravitationally contract to become a main-sequence
supermassive star. Due to the limited gas reservoir in dark matter halos with
10^7 solar masses, the accretion rate onto the central object may drop at late
times, implying the formation of supermassive stars as the typical outcome of
direct collapse. However, if high accretion rates are maintained, a quasi-star
with an interior black hole may form.Comment: 9 pages, 4 figures, submitted to A&A. Comments are welcom
- …