Linear Relation for Wind-Blown Bubble Sizes of Main-Sequence Ob Stars in a Molecular Environment and Implication for Supernova Progenitors

Chen, Yang; Zhou, Ping; Chu, You‐Hua

doi:10.1088/2041-8205/769/1/l16

Cited by 53 publications

(55 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As found by Chen et al (2013), there is a linear relationship between the radius of a main-sequence bubble in a molecular environment (R bubble ) and the initial mass of the energy source star (M star ): R bubble (pc) ≈ 1.22M star /M − 9.16 pc, assuming a constant interclump pressure (see Chen et al 2013 for more details). For the large cavity found in the MWISP observations (major radius of ∼ 0.6 • or 27 pc), a massive star with a mass of ∼ 30 M (O7 or earlier types) is required.…”

Section: Scenario Of a Cavity Produced By Bright Massive Starsmentioning

confidence: 83%

Large-field CO (1–0) observations toward the Galactic historical supernova remnants: a large cavity aroundTycho’s supernova remnant

Chen¹,

Xiong²,

Yang³

2017

A&A

View full text Add to dashboard Cite

Context. The investigation of the interaction between the supernova remnants (SNRs) and interstellar gas is not only necessary to improve our knowledge of SNRs, but also to understand the nature of the progenitor systems. Aims. As a part of the Milky Way Imaging Scroll Painting CO line survey, the aim is to study the interstellar gas surrounding the Galactic historical SNRs. In this work, we present the CO results of Tycho's SNR. Methods. Using the 3×3 Superconducting Spectroscopic Array Receiver (SSAR) at the PMO 13.7-meter telescope, we performed large-field (3 • × 2 • ) and high-sensitivity CO (1-0) molecular line observations toward Tycho's SNR. Results. The CO observations reveal large molecular clouds, stream-like structures, and an inner rim around the remnant. We derived the basic properties (column density, mass, and kinematics) of these objects based on the CO observations. The large molecular clouds individually show an arc toward the remnant center, outlining a large cavity with radii of ∼ 0.3 • × 0.6 • (or 13 pc × 27 pc at a distance of 2.5 kpc) around the remnant. The CO line broadenings and asymmetries detected in the surrounding clouds, the observed expansion of the cavity, in concert with enhanced 12 CO (2-1)/(1-0) intensity ratio detected in previous studies, suggest the interaction of the large cavity with a wind in the region. After excluding the scenario of a large bubble produced by bright massive stars, we suggest that the large cavity could be explained by accretion wind from the progenitor system of Tycho's supernova. Nevertheless, the possibility of the random distribution of a large cavity around Tycho's SNR cannot be ruled out thus far. Further observations are needed to confirm the physical association of the large cavity with Tycho's SNR.

show abstract

Section: Scenario Of a Cavity Produced By Bright Massive Starsmentioning

confidence: 83%

Large-field CO (1–0) observations toward the Galactic historical supernova remnants: a large cavity aroundTycho’s supernova remnant

Chen¹,

Xiong²,

Yang³

2017

A&A

View full text Add to dashboard Cite

show abstract

“…We measured that the cavity radius is about 1.2 pc (1 1 at 3.7 kpc) shown in Figure 10 (left panel). Using the medium density of ∼2×10 3 cm −3 , we infer that the timescale of the ionized cavity is 4.1∼6.3×10 5 years, which is much less than the main-sequence (MS) lifetime of such stars (1.3∼1.6×10 7 years for B1V∼B0.5V stars, Chen et al 2013). Comparing the timescale of the ionized cavity with that of the infrared bubble N61 (9.9 ± 0.2×10 5 years), we suggest that the ionized cavity has been blown via the energetic stellar wind after H II region G34.172+0.175 begin to expand in a filamentary molecular cloud.…”

Section: Infrared Bubbles N61 and N62mentioning

confidence: 96%

“…Because the H II region G34.325+0.211 that created N62 is close to the filamentary molecular cloud, we where R H II is the radius of H II region, n i is the initial number density of gas, and Q Ly is the ionizing luminosity. Assuming the radio continuum emission is optically thin, the ionizing luminosity Q Ly is computed by Condon (1992) n =´n -- Chen et al (2013), we obtain the wind luminosity (L W ) of 0.9∼3.3×10 33 erg s −1 . We measured that the cavity radius is about 1.2 pc (1 1 at 3.7 kpc) shown in Figure 10 (left panel).…”

Section: Infrared Bubbles N61 and N62mentioning

confidence: 99%

Gas Kinematics and Star Formation in the Filamentary Irdc G34.43+0.24

Zhang

et al. 2016

ApJ

View full text Add to dashboard Cite

We performed a multiwavelength study toward the infrared dark cloud (IRDC) G34.43+0.24. New maps of 13 CO J = 1-0 and C 18 O J = 1-0 were obtained from the Purple Mountain Observatory (PMO) 13.7 m radio telescope. At 8 μm (Spitzer-IRAC), IRDC G34.43+0.24 appears to be a dark filament extended by 18′ along the north-south direction. Based on the association with the 870 μm and C 18 O J = 1-0 emission, we suggest that IRDC G34.43+0.24 should not be 18′ in length, but extend to 34′. IRDC G34.43+0.24 contains some massive protostars, UC H II regions, and infrared bubbles. The spatial extend of IRDC G34.43+0.24 is about 37 pc, assuming a distance of 3.7 kpc. IRDC G34.43+0.24 has a linear mass density of ∼1.6×103 M e pc −1 , which is roughly consistent with its critical mass to length ratio. The turbulent motion may help stabilize the filament against the radial collapse. Both infrared bubbles N61 and N62 show a ringlike structure at 8 μm. In particular, N61 has a double-shell structure that has expanded into IRDC G34.43+0.24. The outer shell is traced by 8 μm and 13 CO J = 1-0 emission, while the inner shell is traced by 24 μm and 20 cm emission. We suggest that the outer shell (9.9×10 5 years) is created by the expansion of H II region G34.172+0.175, while the inner shell (4.1∼6.3×10 5 years) may be produced by the energetic stellar wind of its central massive star. From the GLIMPSE I catalog, we selected some Class I sources with an age of ∼10 5 years. These Class I sources are clustered along the filamentary molecular cloud.

show abstract

“…The bubble size of the progenitor of HESS J1731-347 is unknown, as it is for most OB stars in our galaxy because of absorption. Therefore, we adopt the linear relationship between progenitor mass and MS bubble size from Chen et al (2013). Their work is based on 15 well-observed OB stars (8−72 M ) and yields p 1/3 5 R b = α (M/M ) − β pc, where α = 1.22 ± 0.05 and β = 9.16 ± 1.77.…”

Section: Hess J1731-347 Still Residing Inside the Main-sequence Bubblementioning

confidence: 99%

A young supernova remnant illuminating nearby molecular clouds with cosmic rays

Cui

Pühlhofer

Santangelo

2016

A&A

View full text Add to dashboard Cite

The supernova remnant (SNR) HESS J1731-347 displays strong nonthermal TeV γ-ray and X-ray emission, thus the object is presently accelerating particles to very high energies. A distinctive feature of this young SNR is the nearby (∼30 pc in projection) extended source HESS J1729-345, which is currently unidentified but is in spatial projection coinciding with known molecular clouds (MC). We model the SNR evolution to explore whether the TeV emission from HESS J1729-345 can be explained as emission from runaway hadronic cosmic rays (CRs) that are illuminating these MCs. The observational data of HESS J1729-345 and HESS J1731-347 can be reproduced using core-collapse SN models for HESS J1731-347. Starting with different progenitor stars and their presupernova environment, we model potential SNR evolution histories along with the CR acceleration in the SNR and the diffusion of the CRs. A simplified three-dimensional structure of the MCs is introduced based on 12 CO data of that region, adopting a distance of 3.2 kpc to the source. A Monte Carlo based diffusion model for the escaping CRs is developed to deal with the inhomogeneous environment. The fast SNR forward shock speed, as implied from the X-ray data, can easily be explained when employing scenarios with progenitor star masses between 20 M and 25 M , where the SNR shock is still expanding inside the main-sequence (MS) bubble at present time. The TeV spectrum of HESS J1729-345 is satisfactorily fitted by the emission from the highest energy CRs that have escaped the SNR, using a standard Galactic CR diffusion coefficient in the interclump medium. The TeV image of HESS J1729-345 can be explained with a reasonable three-dimensional structure of MCs. The TeV emission from the SNR itself is dominated by leptonic emission in this model. We also explore scenarios where the shock is starting to encounter the dense MS progenitor wind bubble shell. The escaping hadronic CR hypothesis for the γ-ray emission of HESS J1729-345 can still hold, but even in this case our model cannot easily account for the TeV emission from HESS J1731-347 in a hadronic scenario.

show abstract

Linear Relation for Wind-Blown Bubble Sizes of Main-Sequence Ob Stars in a Molecular Environment and Implication for Supernova Progenitors

Cited by 53 publications

References 37 publications

Large-field CO (1–0) observations toward the Galactic historical supernova remnants: a large cavity aroundTycho’s supernova remnant

Large-field CO (1–0) observations toward the Galactic historical supernova remnants: a large cavity aroundTycho’s supernova remnant

Gas Kinematics and Star Formation in the Filamentary Irdc G34.43+0.24

A young supernova remnant illuminating nearby molecular clouds with cosmic rays

Contact Info

Product

Resources

About