Full-disk magnetic oscillations in the solar photosphere

Moretti, P. F.; Cacciani, A.; Hanslmeier, A.; Messerotti, M.; Otruba, W.; Warmuth, A.

doi:10.1051/0004-6361:20030366

Cited by 12 publications

(7 citation statements)

References 24 publications

(28 reference statements)

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“…Down to the flux limit adopted in this analysis (10 −15 erg cm −2 s −1 ), the 2-10 keV counts predicted by the models described in Table 2 are in good agreement with both the counts of the whole sample (including the objects without spectroscopic identifications), and with the Bauer et al (2004) compilation (see Figure 13). The fit of Moretti et al (2003) is also shown. This is an a posteriori test implying that our method, used to correct for the spectroscopic incompleteness of the faint samples, is reliable.…”

Section: The Countsmentioning

confidence: 99%

The HELLAS2XMM Survey. VII. The Hard X‐Ray Luminosity Function of AGNs up toz= 4: More Absorbed AGNs at Low Luminosities and High Redshifts

Franca

Fiore

Comastri

et al. 2005

ApJ

401

139

616

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We have determined the cosmological evolution of the density of active galactic nuclei (AGN) and of their N H distribution as a function of the un-absorbed 2-10 keV luminosity up to redshift 4. We used the HELLAS2XMM sample combined with other published catalogs, yielding a total of 508 AGN. Our best fit is obtained with a luminosity-dependent density evolution (LDDE) model where low luminosity (L X ∼10 43 erg s −1 ) AGN peak at z∼0.7, while high luminosity AGN (L X >10 45 erg s −1 ) peak at z∼2.0. A pure luminosity evolution model (PLE) can instead be rejected.There is evidence that the fraction of absorbed (N H >10 22 cm −2 ) AGN decreases with the intrinsic X-ray luminosity, and increases with the redshift.Our best fit solution provides a good fit to the observed counts, the cosmic X-ray background, and to the observed fraction of absorbed AGN as a function of the flux in the 10 −15 10 44 erg s −1 ) AGN have a density of 267 deg −2 at fluxes S 2−10 >10 −15 erg cm −2 s −1 . Using these results, we estimate a density of supermassive black holes in the local Universe of ρ BH = 3.2 h 2 70 × 10 5 M ⊙ Mpc −3 , which is consistent with the recent measurements of the black hole mass function in the local galaxies.

~~show abstract~~

Section: The Countsmentioning
confidence: 99%

The HELLAS2XMM Survey. VII. The Hard X‐Ray Luminosity Function of AGNs up toz= 4: More Absorbed AGNs at Low Luminosities and High Redshifts
Franca
¹
,
Fiore
²
,
Comastri
³

et al. 2005
ApJ
401
139
616
12
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~~show abstract~~

“…Nevertheless, the instrument we suggest is the only one, to date, whose data have permitted the description in the frequency spectrum associated to the five-minute oscillations (Moretti et al 2003). In this magnetic − ν diagram, the 60-s sampling rate MOF-based system magnetograms demonstrated solar signatures down to 10 8 (G) 2 /Hz.…”

Section: Performancesmentioning
confidence: 76%

“…For some of the scientific results obtained with imaging MOF-based systems, refer to (Warmuth et al 2000;Moretti et al 2001Moretti et al , 2003Moretti et al , 2007Moretti and Severino 2002;Finsterle et al 2004aFinsterle et al , 2004bJefferies et al 2006). …”

Section: Performancesmentioning
confidence: 99%

Future instrumentation for solar physics: a double channel MOF imager on board ASI Space Mission ADAHELI
Moretti¹,
Berrilli
²
,
Bigazzi
³

et al. 2010
Astrophys Space Sci
Self Cite
8
0
4
0
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A Magneto-Optical Filter-based system has been proposed as an optional payload for ASI's low-budget Solar Mission ADAHELI, which has completed its Phase A feasibility study. The instrument is capable of providing simultaneous Dopplergrams, intensity and magnetic solar full-disk maps using the potassium 770 nm and sodium 589 nm solar Fraunhofer lines. The instrument is a version, re-designed for a space environment, of the one which has run an observing campaign at the South Pole in 2008 with unprecedented performance. The MOF-based system we present here is a low-cost, low-weight instrument, thus particularly fit to space applications, capable of providing stability and sensitivity of signals on long-term observations. The instrument will explore regions of the oscillation spectrum not available to other missions' instruments.

~~show abstract~~

“…For instance, in Moretti et al (2001) a first full disk l-ν analysis was performed from a MOF dataset, together with a local analysis, exploring the intensity-velocity phase relation and enabling to investigate the source of solar oscillations. Likewise, in Moretti et al (2003), the magnetic-field-velocity phase difference has been computed, finding evidence of global magnetic oscillations.…”

Section: Introductionmentioning
confidence: 99%

The Tor Vergata Synoptic Solar Telescope (TSST): A robotic, compact facility for solar full disk imaging
Giovannelli
¹
,
Berrilli
²
,
Calchetti
³

et al. 2020
J. Space Weather Space Clim.
6
0
4
0
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By the continuous multi-line observation of the solar atmosphere, it is possible to infer the magnetic and dynamical status of the Sun. This activity is essential to identify the possible precursors of space weather events, such as flare or coronal mass ejections. We describe the design and assembly of TSST (Tor Vergata Synoptic Solar Telescope), a robotic synoptic telescope currently composed of two main full-disk instruments, a H telescope and a Potassium (KI D1) Magneto-Optical Filter (MOF)-based telescope operating at 769.9 nm. TSST is designed to be later upgraded with a second MOF channel. This paper describes the TSST concepts and presents the first light observation carried out in February 2020. We show that TSST is a low-cost robotic facility able to achieve the necessary data for the study of precursors of space weather events (using the magnetic and velocity maps by the MOF telescope) and fast flare detection (by the H telescope) to support Space Weather investigation and services.

~~show abstract~~

Full-disk magnetic oscillations in the solar photosphere

Cited by 12 publications

References 24 publications

The HELLAS2XMM Survey. VII. The Hard X‐Ray Luminosity Function of AGNs up toz= 4: More Absorbed AGNs at Low Luminosities and High Redshifts

The HELLAS2XMM Survey. VII. The Hard X‐Ray Luminosity Function of AGNs up toz= 4: More Absorbed AGNs at Low Luminosities and High Redshifts

Future instrumentation for solar physics: a double channel MOF imager on board ASI Space Mission ADAHELI

The Tor Vergata Synoptic Solar Telescope (TSST): A robotic, compact facility for solar full disk imaging

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