<i>Herschel </i>observations of the circumstellar environments  of the Herbig Be stars R Mon and PDS 27

Jiménez-Donaire, María J.; Meeus, G.; Karska, A.; Montesinos, B.; Bouwman, J.; Eiroa, C.; Henning, Thomas

doi:10.1051/0004-6361/201629053

Cited by 11 publications

(6 citation statements)

References 66 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…3.2, Karska et al 2013, Nisini et al 2015; (ii) broad molecular line profiles with velocities up to ∼50 km s −1 (Kristensen et al 2012, 2017b, San José-García et al 2013, Mottram et al 2014; (iii) a universal CO rotational temperature of ∼300 K, independent of protostellar luminosity (see Sec. 4.1, Manoj et al 2013, Matuszak et al 2015, Jiménez-Donaire et al 2017; (iv) an overall cooling budget in far-IR lines similar to predictions of stationary C type shocks (see Sect. 4.2, Karska et al 2013, Lee et al 2014a.…”

Section: Origin Of Far-ir Emission In Fuv-irradiated C-shockssupporting

confidence: 65%

The Herschel-PACS Legacy of Low-mass Protostars: The Properties of Warm and Hot Gas Components and Their Origin in Far-UV Illuminated Shocks

Karska

Kaufman

Kristensen

et al. 2018

ApJS

118

View full text Add to dashboard Cite

Recent observations from Herschel allow the identification of important mechanisms responsible for the heating of gas surrounding low-mass protostars and its subsequent cooling in the far-infrared (FIR). Shocks are routinely invoked to reproduce some properties of the far-IR spectra, but standard models fail to reproduce the emission from key molecules, e.g. H 2 O. Here, we present the Herschel-PACS far-IR spectroscopy of 90 embedded low-mass protostars (Class 0/I). The Herschel-PACS spectral maps covering ∼ 55 − 210 µm with a field-of-view of ∼50" are used to quantify the gas excitation conditions and spatial extent using rotational transitions of H 2 O, high-J CO, and OH, as well as [O I] and [C II]. We confirm that a warm (∼300 K) CO reservoir is ubiquitous and that a hotter component (760 ± 170 K) is frequently detected around protostars. The line emission is extended beyond ∼1000 AU spatial scales in 40/90 objects, typically in molecular tracers in Class 0 and atomic tracers in Class I objects. High-velocity emission ( 90 km s −1 ) is detected in only 10 sources in the [O I] line, suggesting that the bulk of [O I] arises from gas that is moving slower than typical jets. Line flux ratios show an excellent agreement with models of C-shocks illuminated by UV photons for pre-shock densities of ∼10 5 cm −3 and UV fields 0.1-10 times the interstellar value. The far-IR molecular and atomic lines are a unique diagnostic of feedback from UV emission and shocks in envelopes of deeply embedded protostars.

show abstract

Section: Origin Of Far-ir Emission In Fuv-irradiated C-shockssupporting

confidence: 65%

The Herschel-PACS Legacy of Low-mass Protostars: The Properties of Warm and Hot Gas Components and Their Origin in Far-UV Illuminated Shocks

Karska

Kaufman

Kristensen

et al. 2018

ApJS

118

View full text Add to dashboard Cite

show abstract

“…In addition, 23 sources cannot be classified because photometry was not available in the relevant ranges. It is also noted that the IRAS bands may be contaminated by the environment close to some stars (Verhoeff et al 2012;Jiménez-Donaire et al 2017), which may affect the M01 group assignment.…”

Section: Sed Classificationmentioning

confidence: 99%

Homogeneous study of Herbig Ae/Be stars from spectral energy distributions and Gaia EDR3

Guzmán-Díaz

Mendigutía

Montesinos

et al. 2021

A&A

Self Cite

View full text Add to dashboard Cite

Context. Herbig Ae/Be stars (HAeBes) have so far been studied based on relatively small samples that are scattered throughout the sky. Their fundamental stellar and circumstellar parameters and statistical properties were derived with heterogeneous approaches before Gaia. Aims. Our main goal is to contribute to the study of HAeBes from the largest sample of such sources to date, for which stellar and circumstellar properties have been determined homogeneously from the analysis of the spectral energy distributions (SEDs) and Gaia EDR3 parallaxes and photometry. Methods. Multiwavelength photometry was compiled for 209 bona fide HAeBes for which Gaia EDR3 distances were estimated. Using the Virtual Observatory SED Analyser (VOSA), photospheric models were fit to the optical SEDs to derive stellar parameters, and the excesses at infrared (IR) and longer wavelengths were characterized to derive several circumstellar properties. A statistical analysis was carried out to show the potential use of such a large dataset. Results. The stellar temperature, luminosity, radius, mass, and age were derived for each star based on optical photometry. In addition, their IR SEDs were classified according to two different schemes, and their mass accretion rates, disk masses, and the sizes of the inner dust holes were also estimated uniformly. The initial mass function fits the stellar mass distribution of the sample within 2 < M*∕M⊙ < 12. In this aspect, the sample is therefore representative of the HAeBe regime and can be used for statistical purposes when it is taken into account that the boundaries are not well probed. Our statistical study does not reveal any connection between the SED shape from the Meeus et al. (2001, A&A, 365, 476) classification and the presence of transitional disks, which are identified here based on the SEDs that show an IR excess starting at the K band or longer wavelengths. In contrast, only ~28% of the HAeBes have transitional disks, and the related dust disk holes are more frequent in HBes than in HAes (~34% vs. 15%). The relatively small inner disk holes and old stellar ages estimated for most transitional HAes indicate that photoevaporation cannot be the main mechanism driving disk dissipation in these sources. In contrast, the inner disk holes and ages of most transitional HBes are consistent with the photoevaporation scenario, although these results alone do not unambiguously discard other disk dissipation mechanisms. Conclusions. The complete dataset is available online through a Virtual Observatory-compliant archive, representing the most recent reference for statistical studies on the HAeBe regime. VOSA is a complementary tool for the future characterization of newly identified HAeBes.

show abstract

“…It is also higher than the turbulent velocities observed in other Herbig Ae and T Tauri disks (see, e.g., Piétu et al 2007). Therefore, we consider that the high J u = 14–30 CO line fluxes are better explained by some contribution from the envelope and/or outflow to the emission of these lines (Jiménez-Donaire et al 2017). Taking into account that these lines are unresolved with the PACS spectral and spatial resolution, we favor the interpretation of some contribution from the inner envelope and/or the UV-illuminated walls of the molecular outflow to the J u = 14-30 lines (Karska et al 2014).…”

Section: Disk Model: 12co and 13co Linesmentioning

confidence: 99%

Revisiting the case of R Monocerotis: Is CO removed at R < 20 au?

Alonso-Albi

Riviére-Marichalar

Fuente

et al. 2018

A&A

Self Cite

View full text Add to dashboard Cite

Context To our knowledge, R Mon is the only B0 star in which a gaseous Keplerian disk has been detected. However, there is some controversy about the spectral type of R Mon. Some authors propose that it could be a later B8e star, where disks are more common. Aims Our goal is to re-evaluate the R Mon spectral type and characterize its protoplanetary disk. Methods The spectral type of R Mon has been re-evaluated using the available continuum data and UVES emission lines. We used a power-law disk model to fit previous 12CO 1→0 and 2→1 interferometric observations and the PACS CO data to investigate the disk structure. Interferometric detections of 13CO J=1→0, HCO+ 1→0, and CN 1→0 lines using the IRAM Plateau de Bure Interferometer (PdBI) are presented. The HCN 1→0 line was not detected. Results Our analysis confirms that R Mon is a B0 star. The disk model compatible with the 12CO 1→0 and 2→1 interferometric observations falls short of predicting the observed fluxes of the 1431 CO lines suggest the existence of a region empty of CO at R≲20 au in the proto-planetary disk. The intense emission of the HCO+ and CN lines shows the strong influence of UV photons on gas chemistry. Conclusions The observations gathered in this paper are consistent with the presence of a transition disk with a cavity of Rin≳20 au around R Mon. This size is similar to the photoevaporation radius that supports the interpretation that UV photoevaporation is main disk dispersal mechanism in massive stars

show abstract

Herschel observations of the circumstellar environments of the Herbig Be stars R Mon and PDS 27

Cited by 11 publications

References 66 publications

The Herschel-PACS Legacy of Low-mass Protostars: The Properties of Warm and Hot Gas Components and Their Origin in Far-UV Illuminated Shocks

The Herschel-PACS Legacy of Low-mass Protostars: The Properties of Warm and Hot Gas Components and Their Origin in Far-UV Illuminated Shocks

Homogeneous study of Herbig Ae/Be stars from spectral energy distributions and Gaia EDR3

Revisiting the case of R Monocerotis: Is CO removed at R < 20 au?

Contact Info

Product

Resources

About