Dust and Polycyclic Aromatic Hydrocarbon in the Hd 34700 Debris Disk

Seok, Ji Yeon; Li, Aigen

doi:10.1088/0004-637x/809/1/22

Cited by 11 publications

(27 citation statements)

References 57 publications

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“…For each source, the peak wavelengths and widths of some of the Drude profiles are slightly modified to be consistent with the observed spectrum. In this way, the observed residual spectra can be fitted more closely (e.g., see Seok & Li 2015. Note that the integrated area of each Drude profile is kept unchanged so that the model calculations are coherent through the entire sample.…”

Section: Modelmentioning

confidence: 99%

“…For those with T eff 6, 000 K, β RP is expected to be larger than unity, which implies that PAHs would be continuously expelled outward from the disk. The timescale of the RP (τ RP ) expelling can be estimated by adopting the local dynamical timescale (τ dyn , see Li & Lunine 2003;Seok & Li 2015). We calculate τ dyn = 2π/Ω(r), where Ω(r) ≡ (GM ⋆ /r 3 ) 1/2 is the Keplerian frequency.…”

Section: Destruction Of Pahs In Ppdsmentioning

confidence: 99%

“…The HD 34700 system composed of a spectroscopic binary (Torres 2004) and two other faint components is confirmed with JHK-band images and optical spectroscopy . Although it has not been spatially resolved, analysis of its SED indicates the dust spatial distribution of the HD 34700 disk peaks at ≈ 100 AU and decreases outward with a power-law index of ≈ 2 (Seok & Li 2015). The PAH parameters derived in this work ( a 0 = 2.5 ± 0.5Å, σ = 0.3 ± 0.1, and φ ion = 0.2 ± 0.1) are consistent with the previous results from Seok & Li (2015), which indicate small PAH population (a 0 = 3.5Å and σ = 0.3) with a mixture of neutral and ionized PAHs: for small PAHs (a 5Å), φ ion ∼ 0.2 at r = 25 AU (see their Figure 3).…”

Section: A9 Hd 34700mentioning

confidence: 99%

“…-(1) Alecian et al (2013), (2) Rigliaco et al (2015), (9) Sturm et al (2013), (10) Seok & Li (2015), (11) Maaskant et al (2014), (12) Juhász et al (2010), (13) Fairlamb et al (2015), (14) Mariñas et al (2011), (15) Verhoeff et al (2012), (16) van Boekel et al (2005), (17) Siebenmorgen et al (2000), (18) Hubrig et al (2009), (19) Folsom et al (2012, (20) Fukagawa et al (2010), (21) Seok & Li (2016), (22) Keller et al (2008), (23) Merín et al (2010), (24) Harvey et al (1984), (25) Kóspál et al(2012), (26) Boersma et al (2009), (27) Brown et al (2008), (28) Borges Fernandes et al (2007, (29) Schütz et al (2009), (30) Prato et al (2003), (31) Jeffers et al (2013), (32) Huélamo et al (2011), (33) Casey et al (1998), (34) Pinilla et al (2014), (35) Magazzu et al (1991), (36) Liu et al (2011), (37) …”

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confidence: 99%

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Polycyclic Aromatic Hydrocarbons in Protoplanetary Disks around Herbig Ae/Be and T Tauri Stars

Seok¹,

Li²

2017

ApJ

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A distinct set of broad emission features at 3. 3, 6.2, 7.7, 8.6, 11.3, and 12.7 µm, is often detected in protoplanetary disks (PPDs). These features are commonly attributed to polycyclic aromatic hydrocarbons (PAHs). We model these emission features in the infrared spectra of 69 PPDs around 14 T Tauri and 55 Herbig Ae/Be stars in terms of astronomical-PAHs. For each PPD, we derive the size distribution and the charge state of PAHs. We then examine the correlations of the PAH properties (i.e., sizes and ionization fractions) with the stellar properties (e.g., stellar effective temperature, luminosity, and mass). We find that the characteristic size of PAHs shows a tendency of correlating with the stellar effective temperature (T eff ) and interpret this as the preferential photodissociation of small PAHs in systems with higher T eff of which the stellar photons are more energetic. In addition, the PAH size shows a moderate correlation with the red-ward wavelength-shift of the 7.7 µm PAH feature that is commonly observed in disks around cool stars. The ionization fraction of PAHs does not seem to correlate with any stellar parameters. This is because the charging of PAHs depends on not only the stellar properties (e.g., T eff , luminosity) but also the spatial distribution of PAHs in the disks. The mere negative correlation between the PAH size and the stellar age suggests that continuous replenishment of PAHs via the outgassing of cometary bodies and/or the collisional grinding of planetesimals and asteroids is required to maintain the abundance of small PAHs against complete destruction by photodissociation.

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Section: Modelmentioning

confidence: 99%

Section: Destruction Of Pahs In Ppdsmentioning

confidence: 99%

Section: A9 Hd 34700mentioning

confidence: 99%

mentioning

confidence: 99%

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Polycyclic Aromatic Hydrocarbons in Protoplanetary Disks around Herbig Ae/Be and T Tauri Stars

Seok¹,

Li²

2017

ApJ

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“…The 6.85 and 7.25 µm aliphatic C-H deformation bands are labelled in (e) and (f) for protoplanetary disks. The sharp gaseous emission lines are labelled in (g) 178,179 .…”

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confidence: 99%

Spitzer’s perspective of polycyclic aromatic hydrocarbons in galaxies

2020

Nat Astron

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160

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Polycyclic aromatic hydrocarbon (PAH) molecules, as revealed by the distinctive set of emission bands at 3. 3, 6.2, 7.7, 8.6, 11.3 and 12.7 µm characteristic of their vibrational modes, are abundant and widespread throughout the Universe. They are ubiquitously seen in a wide variety of astrophysical regions, ranging from planet-forming disks around young stars to the interstellar medium (ISM) of the Milky Way and external galaxies out to high redshifts at z > ∼ 4. PAHs profoundly influence the thermal budget and chemistry of the ISM by dominating the photoelectric heating of the gas and controlling the ionization balance. Here, we review the current state of knowledge of the astrophysics of PAHs, focusing on their observational characteristics obtained from the Spitzer Space Telescope and their diagnostic power for probing the local physical and chemical conditions and processes. Special attention is paid to the spectral properties of PAHs and their variations revealed by the Infrared Spectrograph (IRS) on board Spitzer across a much broader range of extragalactic environments (e.g., distant galaxies, early-type galaxies, galactic halos, active galactic nuclei, and low-metallicity galaxies) than was previously possible with the Infrared Space Observatory (ISO) or any other telescope facilities. Also highlighted is the relation between the PAH abundance and the galaxy metallicity established for the first time by Spitzer.

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Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): HD 34700 A unveils an inner ring

Columba,

Rigliaco,

Gratton

et al. 2024

A&A

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Context. The study of protoplanetary disks is fundamental to understand their evolution and interaction with the surrounding environment, and to constrain planet formation mechanisms. Aims. We aim to characterise the young binary system HD 34700 A, which shows a wealth of structures. Methods. Taking advantage of the high-contrast imaging instruments SPHERE at the VLT, LMIRCam at the LBT, and of ALMA observations, we analyse this system at multiple wavelengths. We study the morphology of the rings and spiral arms and the scattering properties of the dust. We discuss the possible causes of all the observed features. Results. We detect for the first time, in the Hα band, a ring extending from ~65 au to ~120 au, inside the ring which is already known from recent studies. These two have different physical and geometrical properties. Based on the scattering properties, the outer ring may consist of grains with a typical size of aout ≥ 4 µm, while the inner ring has a smaller typical size of ain ≤ 0.4 µm. Two extended logarithmic spiral arms stem from opposite sides of the disk. The outer ring appears as a spiral arm itself, with a variable radial distance from the centre and extended substructures. ALMA data confirm the presence of a millimetric dust substructure centred just outside the outer ring, and detect misaligned gas rotation patterns for HD 34700 A and B. Conclusions. The complexity of HD 34700 A, revealed by the variety of observed features, suggests the existence of one or more disk-shaping physical mechanisms. Our findings are compatible with the presence inside the disk of an as of yet undetected planet of several Jupiter masses and the system interaction with the surroundings, by means of gas cloudlet capture or flybys. Further observations with JWST/MIRI or ALMA (gas kinematics) could shed more light on them.

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Dust and Polycyclic Aromatic Hydrocarbon in the Hd 34700 Debris Disk

Cited by 11 publications

References 57 publications

Polycyclic Aromatic Hydrocarbons in Protoplanetary Disks around Herbig Ae/Be and T Tauri Stars

Polycyclic Aromatic Hydrocarbons in Protoplanetary Disks around Herbig Ae/Be and T Tauri Stars

Spitzer’s perspective of polycyclic aromatic hydrocarbons in galaxies

Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): HD 34700 A unveils an inner ring

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