Energetic feedback and<sup>26</sup>Al from massive stars and their supernovae in the Carina region

Voss, R.; Martin, Pierrick; Diehl, R.; Hartmann, D. H.; Preibisch, Thomas

doi:10.1051/0004-6361/201118209

Cited by 36 publications

(47 citation statements)

References 46 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Thus, our simulations apply, within the limitations outlined in Sect. 4 above, well to hierarchically clustered star formation complexes like the Orion (Voss et al 2010), Scorpius-Centaurus or Carina (Voss et al 2012) regions.…”

Section: Discussionmentioning

confidence: 81%

“…Later, the energy input is dominated by supernovae. Observed subgroups have an age difference of the order of a few Myr (Voss et al 2010(Voss et al , 2012). Thus, it appears possible that the energy response (compare Eq.…”

Section: Discussionmentioning

confidence: 96%

“…Observations find energy responses of about ten per cent or higher (e.g. Oey & García-Segura 2004;Voss et al 2012). This agrees very well with the results in the wind phase of our highest resolution run and might suggest that additional effects, which are not taken into account in our simulation and which we believe should only increase the energy response, may not dominate.…”

Section: Discussionmentioning

confidence: 99%

See 2 more Smart Citations

Feedback by massive stars and the emergence of superbubbles

Krause

Fierlinger

Diehl

et al. 2013

A&A

Self Cite

113

View full text Add to dashboard Cite

Context. Massive stars influence their environment through stellar winds, ionising radiation, and supernova explosions. This is signified by observed interstellar bubbles. Such feedback is an important factor for galaxy evolution theory and galactic wind models. The efficiency of the energy injection into the interstellar medium (ISM) via bubbles and superbubbles is uncertain, and is usually treated as a free parameter for galaxy scale effects. In particular, since many stars are born in groups, it is interesting to study the dependence of the effective energy injection on the concentration of the stars. Aims. We aim to reproduce observations of superbubbles, their relation to the energy injection of the parent stars, and to understand their effective energy input into the ISM, as a function of the spatial configuration of the group of parent stars. Methods. We study the evolution of isolated and merging interstellar bubbles of three stars (25, 32, and 60 M ) in a homogeneous background medium with a density of 10m p cm −3 via 3D-hydrodynamic simulations with standard ISM thermodynamics (optically thin radiative cooling and photo-electric heating) and time-dependent energy and mass input according to stellar evolutionary tracks. We vary the position of the three stars relative to each other to compare the energy response for cases of isolated, merging and initially cospatial bubbles. Results. Mainly due to the Vishniac instability, our simulated bubbles develop thick shells and filamentary internal structures in column density. The shell widths reach tens of per cent of the outer bubble radius, which compares favourably to observations. More energy is retained in the ISM for more closely packed groups, by up to a factor of three and typically a factor of two for intermediate times after the first supernova. Once the superbubble is established, different positions of the contained stars make only a minor difference to the energy tracks. For our case of three massive stars, the energy deposition varies only very little for distances up to about 30 pc between the stars. Energy injected by supernovae is entirely dissipated in a superbubble on a timescale of about 1 Myr, which increases slightly with the superbubble size at the time of the explosion. Conclusions. The Vishniac instability may be responsible for the broadening of the shells of interstellar bubbles. Massive star winds are significant energetically due to their -in the long run -more efficient, steady energy injection and because they evacuate the space around the massive stars. For larger scale simulations, the feedback effect of close groups of stars or clusters may be subsumed into one effective energy input with insignificant loss of energy accuracy.

show abstract

Section: Discussionmentioning

confidence: 81%

Section: Discussionmentioning

confidence: 96%

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Feedback by massive stars and the emergence of superbubbles

Krause

Fierlinger

Diehl

et al. 2013

A&A

Self Cite

113

View full text Add to dashboard Cite

show abstract

“…Indeed, star-forming regions are observed to be actively clearing away gas at an age of about 10 6 years (e.g. Voss et al 2010Voss et al , 2012Preibisch et al 2012;Galván-Madrid et al 2013;Klaassen et al 2014), and to be free of dense gas from about a few Myr after the onset of star formation (e.g., the review by Lada & Lada 2003).…”

Section: Introductionmentioning

confidence: 99%

Gas expulsion in massive star clusters?

Krause

Charbonnel

Bastian

et al. 2016

A&A

View full text Add to dashboard Cite

Context. Gas expulsion is a central concept in some of the models for multiple populations and the light-element anti-correlations in globular clusters. If the star formation efficiency was around 30 per cent and the gas expulsion happened on the crossing timescale, this process could preferentially expel stars born with the chemical composition of the proto-cluster gas, while stars with special composition born in the centre would remain bound. Recently, a sample of extragalactic, gas-free, young massive clusters has been identified that has the potential to test the conditions for gas expulsion. Aims. We investigate the conditions required for residual gas expulsion on the crossing timescale. We consider a standard initial mass function and different models for the energy production in the cluster: metallicity-dependent stellar winds, radiation, supernovae and more energetic events, such as hypernovae, which are related to gamma ray bursts. The latter may be more energetic than supernovae by up to two orders of magnitude. Methods. We computed a large number of thin-shell models for the gas dynamics, and calculated whether the Rayleigh-Taylor instability is able to disrupt the shell before it reaches the escape speed. Results. We show that the success of gas expulsion depends on the compactness index of a star cluster C 5 ≡ (M * /10 5 M )/(r h /pc), with initial stellar mass M * and half-mass radius r h . For given C 5 , a certain critical, local star formation efficiency is required to remove the rest of the gas. Common stellar feedback processes may not lead to gas expulsion with significant loss of stars above C 5 ≈ 1. Considering pulsar winds and hypernovae, the limit increases to C 5 ≈ 30. If successful, gas expulsion generally takes place on the crossing timescale. Some observed young massive clusters have 1 < C 5 < 10 and are gas-free at ≈10 Myr. This suggests that gas expulsion does not affect their stellar mass significantly, unless powerful pulsar winds and hypernovae are common in such objects. By comparison to observations, we show that C 5 is a better predictor for the expression of multiple populations than stellar mass. The best separation between star clusters with and without multiple populations is achieved by a stellar winds-based gas expulsion model, where gas expulsion would occur exclusively in star clusters without multiple populations. Single and multiple population clusters also have little overlap in metallicity and age. Conclusions. Globular clusters should initially have C 5 100, if the gas expulsion paradigm was correct. Early gas expulsion, which is suggested by the young massive cluster observations, hence would require special circumstances, and is excluded for several objects. Most likely, the stellar masses did not change significantly at the removal of the primordial gas. Instead, the predictive power of the C 5 index for the expression of multiple populations is consistent with the idea that gas expulsion may prevent the expression of multiple populations. On this bas...

show abstract

“…18), and provide a more specific test for massive-star models than can be obtained from Galaxy-wide analysis as discussed above. With deeper exposure, this became possible in the late INTEGRAL mission for the Cygnus [85], Carina [140], and Scorpius-Centaurus [28] regions; for other candidate locations of massivestar groups INTEGRAL's sensitivity is insufficient, due to their fainter 26 Al emission.…”

Section: Special Regionsmentioning

confidence: 99%

Cosmic Gamma-Ray Spectroscopy

Diehl

2013

Astronomical Review

View full text Add to dashboard Cite

Penetrating gamma-rays require complex instrumentation for astronomical spectroscopy measurements of gamma-rays from cosmic sources. Multiple-interaction detectors in space combined with sophisticated postprocessing of detector events on ground have lead to a spectroscopy performance which is now capable to provide new astrophysical insights. Spectral signatures in the MeV regime originate from transitions in the nuclei of atoms (rather than in their electron shell). Nuclear transitions are stimulated by either radioactive decays or high-energy nuclear collisions such as with cosmic rays. Gamma-ray lines have been detected from radioactive isotopes produced in nuclear burning inside stars and supernovae, and from energetic-particle interactions in solar flares. Radioactive-decay gamma-rays from 56 Ni directly reflect the source of supernova light. 44 Ti is produced in core-collapse supernova interiors, and the paucity of corresponding 44 Ti gamma-ray line sources reflects the variety of dynamical conditions herein. 26 Al and 60 Fe are dispersed in interstellar space from massive-star nucleosynthesis over millions of years. Gamma-rays from their decay are measured in detail by gamma-ray telescopes, astrophysical interpretations reach from massive-star interiors to dynamical processes in the interstellar medium. Nuclear de-excitation gamma-ray lines have been found in solar-flare events, and convey information about energetic-particle production in these events, and their interaction in the solar atmosphere. The annihilation of positrons leads to another type of cosmic gamma-ray source. The characteristic annihilation gamma-rays at 511 keV have been measured long ago in solar flares, and now throughout the interstellar medium of our Milky Way galaxy. But now a puzzle has appeared, as a surprising predominance of the central bulge region was determined. This requires either new positron sources or transport processes not yet known to us. In this paper we discuss instrumentation and data processing for cosmic gamma-ray spectroscopy, and the astrophysical issues and insights from these measurements.

show abstract

Energetic feedback and²⁶Al from massive stars and their supernovae in the Carina region

Cited by 36 publications

References 46 publications

Feedback by massive stars and the emergence of superbubbles

Feedback by massive stars and the emergence of superbubbles

Gas expulsion in massive star clusters?

Cosmic Gamma-Ray Spectroscopy

Contact Info

Product

Resources

About

Energetic feedback and26Al from massive stars and their supernovae in the Carina region

Cited by 36 publications

References 46 publications

Feedback by massive stars and the emergence of superbubbles

Feedback by massive stars and the emergence of superbubbles

Gas expulsion in massive star clusters?

Cosmic Gamma-Ray Spectroscopy

Contact Info

Product

Resources

About

Energetic feedback and²⁶Al from massive stars and their supernovae in the Carina region