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\begin{titlepage}

\mbox{  }

\vspace{5cm}

\begin{flushright}
{\Huge \bf Resume}
\rule{\textwidth}{2mm}

\vspace{0.5cm}

%{\Large \textit{Życiorys naukowy i wykaz publikacji}}


\vspace{6cm}

{\Large Agnieszka Kryszczyńska}

\vspace{5cm}

Institute Astronomical Observatory \\
Adam Mickiewicz University\\
Poznań

\vspace{1.5cm}

{Poznań, 2013}

\end{flushright}
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\cleardoublepage

\section{CV}

\subsection{Personal data}
\begin{itemize}\setlength{\itemsep}{-0.4\baselineskip}
\item Name and surname: Agnieszka Kryszczyńska

\item Place of work: Institute Astronomical Observatory, \\
      Adam Mickiewicz University,\\ 
      Słoneczna 36, 60-286 Poznań,\\
      tel. +48 61 829 2783,\\
      e-mail: agn@amu.edu.pl 
\end{itemize}

\subsection{Education and scientific degrees}

\begin{itemize}\setlength{\itemsep}{-0.4\baselineskip}
\item 1983-1988 -- Studies of physics, specialisation astrometry, 
      Department of Mathematics and Physics,
      Adam Mickiewicz University, Poznań

\item 1989 -- Master degree, thesis  
      {\it Determination of asteroid diameters}, 
      supervisor -- prof.~dr~hab. Hieronim Hurnik 

\item 1998 -- Ph.D. in physical sciences, thesis  
      {\it Rotation and precession of asteroids in comparison with the observed 
      and modelled lightcurves}, Department of Physics and Astronomy, 
      Nicolas Copernicus University Toruń, supervisor -- 
      prof.~dr~hab. Taduesz Michałowski
\end{itemize}

\subsection{Information about employment}

\begin{itemize}\setlength{\itemsep}{-0.4\baselineskip}
\item 01.10.1988 --- 31.01.1990 --- astronomer, Astronomical Observatory, 
      Adam Mickiewicz University

\item 01.02.1990 --- 30.09.1998 --- assistant, Astronomical Observatory, 
      Adam Mickiewicz University

\item od 01.10.1998 --- assistant professor, Institute Astronomical Observatory, 
      Adam Mickiewicz University 

\end{itemize}

\section{Scientific achievement --- base of the \\ habilitation procedure }

My scientific achievement is a series of publications entitled\\
{\bf ,,Observational verification of the influence of the Yarkovsky and YORP effects 
on asteroids''}.

\subsection{List of publications underlying the habilitation procedure \\
}

\begin{enumerate}
\item [H1] 
La Spina A., Paolicchi P., {\bf Kryszczyńska A.}, Pravec P. 2004. \\
Retrograde spins of near-Earth asteroids from the Yarkovsky effect.\\
{\it Nature} 428, 400-401, IF(2004)=32.182, \\
\textit{Publication is based on the ,,Asteroid spin vector determinations database''
maintained by myself, I prapared data for statistical analysis, proposed separate 
approach to the NEAs and Main Belt Asteroids, took part in the interpretation of the 
results and writing the text of the paper, own contribution 30\%.}

\item [H2]
{\bf Kryszczyńska A.}, La Spina A., Paolicchi P., Harris A.W., Breiter S.,
Pravec P. 2007. \\
New findings on asteroid spin-vector distribution. \\
{\it Icarus} 192, 223-237, IF(2007)=2.869,  \\
\textit{Publication is based on the ,,Asteroid spin vector determinations database''
maintained by myself, I prapared data for statistical analysis, 
took part in the interpretation of the results and wrote 80\% of the text of the paper, 
own contribution 75\%.}

\item [H3]
{\bf Kryszczyńska, A.}, Colas F., Descamps P., Bartczak P., Polińska M.,
Kwiatkowski T., Lecacheux J., Hirsch R., Fagas M., Kamiński K., Michałowski T., 
Marciniak A. 2009. \\
New binary asteroid 809 Lundia. I. Photometry and modelling.\\
{\it Astronomy and Astrophysics} 501, 769-776, IF(2009)=4.179,\\
\textit{I discovered binary nature of the asteroid 809 Lundia, organized observing 
campaign of this object, prepared data for modelling, interpreted results of modelling,
wrote 80\% of the text of the publication, own contribution 70\%.}

\item [H4]
{\bf Kryszczyńska A.}, Colas F., Polińska M., Hirsch R., Ivanova V. Apostolovska G., 
Bilkina B., Velichko F. P., Kwiatkowski T., Kankiewicz P., Vachier F., Umlenski V., 
Michałowski T., Marciniak A., Maury A., Kamiński K., Fagas M., Dimitrov W., 
Borczyk W., Sobkowiak K., Lecacheux J., Behrend R., Klotz A., Bernasconi L., 
Crippa R., Manzini F., Poncy R., Antonini P., Oszkiewicz D., Santana-Ros T. 
2012. \\
Do Slivan states exist in the Flora family? I. Photometric survey of the 
Flora region. \\
{\it Astronomy and Astrophysics} 546, A72, IF(2012)=5.084, \\
\textit{I organized the observing campaign of the Flora family asteroids, observed a part
of the objects, coordinated the rest of observations, reduced the photometric data, determined 
the spin periods of the observed asteroids, interpreted results and wrote the whole text
of the publication, own contribution 70\%.}

\item [H5]
{\bf Kryszczyńska A.}, 2013. \\
Do Slivan states exist in the Flora family? II. 
Fingerprints of the Yarkovsky and YORP effects. \\
{\it Astronomy and Astrophysics} 551, A102, IF(2012)=5.084  \\
\textit{I prepared data for modelling, modelled all described bodies, interpreted results,
wrote the whole text of the publication, own contribution 100\%.}

\end{enumerate}

\subsection{Description of the scientific goals of the listed publications and the obtained results}

Non-gravitational effects connected with the influence of the solar radiation on asteroids 
were a subject of intensive studies during last two decades. These effects are called Yarkovsky
and YORP. The theory and our understanding of the Yarkovsky effect seems to be good
but the theory of the YORP effect requires sustantial improvement.  
In such context observational works which can verify theoretical asumptions are of great importance.
The publications H1-H5 mentioned above are devoted to this issue.

For many years the collisional evolution of the main belt was claimed as a main process
forming asteroids spin properties. Latest observations and theoretical analysis show that 
the the situation is different and that the Yarkovsky and YORP effects might be the main processes
influencing dynamical properties of asteroids.

In 1901 the effect connected with the difference between the directions of the sunlight and the 
reemitted light by a rotating body, mainly in infrared, was described by Jan Jarkowski 
(the effects is known as Yarkovsky).
The delay in the reemision depends on the surface properties of the body.
The recoil force depends on the position of the spin axis and direction of the rotation of the body.


\begin{figure}
\centering
\includegraphics[width=4.5cm,height=10cm,angle=-90]{yarko1.ps}
\caption{Yarkovsky effect. An asteroid is warmed by sunlight, its afternoon side becoming hottest. 
As a result, that face of the asteroid re-radiates most thermal radiation, creating a recoil 
force on the asteroid and causing it to drift a little. The direction of the radiation depends 
on whether the asteroid is rotating in a prograde (anticlockwise) manner (a) or in a retrograde 
(clockwise) manner (b). Nature 425, 131.}
\label{rys1}
\end{figure}


In case of prograde rotators (like the Earth) the Yarkovky effect causes expanding of orbits.
In case of retrograde rotators the orbit shrinks (Fig.1).
The Yarkovsky drift is the most effective for objects smaller than 40~km, and neglectable for 
planets and objects smaller than 10~cm.                                               

Re-radiation of the absorbed sunlight influences not only the orbital motion but also modifies the spin 
axis orientation and spin rate.  The name YORP effect comes from an abbreviation of the names 
Yarkovsky-O’Keefe-Radzievskii-Paddack, a listing of scientists who worked on or inspired 
the idea that radiation-driven accelerations could modify the rotation rates and spin axis orientation 
of small planetary bodies. The effect depends on the size and shape of the body (does not work on 
spherical or ellipsoidal bodies), thermal parameters of the surface (thermal conductivity), 
and distance from the Sun. The YORP effect may spin up or spin down rotation and forces the spin axis 
to become perpendicular to the orbital plane.

Orbital parameters of asteroids are known for more than 600~000 objects, however the position of the 
spin vector, the sidereal period of rotation and shape is known only for about 200 bodies.  
Determination of the complete asteroid model requires many years of photometric observations, usage of 
radar, adaptive optics or space missions.
Rotational parameters of asteroids up to 1995 were collected by P. Magnusson from Uppsala Observatory 
(Sweden). Unfortunately no update of the spin vector collection was released in the years 1995--2002.
Feeling the need to continue the Magnusson's work in 2002, with his agreement, I took over his database.
The current version of the ''Asteroid spin vector determinations database'' and its regular updates are 
available at the website of the Astronomical Observatory of A. Mickiewicz University:\\
{\verb http://www.astro.amu.edu.pl/Science/Asteroids/ }.    \\

\begin{figure}
\begin{center}
\includegraphics[width=9cm,height=7cm]{aaang.eps}
\end{center}
\caption{Latitude distributions for MB asteroids and NEAs. The histogram shows (solid
line) the distribution of the ecliptic latitude for the poles of NEAs. The distribution 
is compared to MB asteroids (dashed line), which has been normalized to the same number of
objects.}
\end{figure}

The decision of the collecting of asteroids rotational parameters was very successful.
The publications H1 and H2 were done on the basis of the new asteroids spin vector collection.

Just before the conference Asteroids Comets Meteors 2002, Prof. Paolo Paolicchi and Dr. Alessandra 
La Spina from Pisa University, offered me a proposal of new statistical studies of rotational 
parameters of asteroids based on my updated spin vector determinations dataset.
I suggested to divide our studies into two parts and separately analyse the main belt asteroids (MBAs)
and near Earth asteroids (NEAs).

Dynamical resonances in the main belt are a gateway for production of NEAs.
The major resonances 3:1 or 2:1 with Jupiter or secular resonance $\nu_6$ with Saturn
are considered as preferential channels. 
Collisional evolution have long been claimed as possible process of reaching the resonant orbits.
In such case the distribution of spin vectors among NEAs should be random.
If the Yarkovsky drift dominates reaching of the resonances the theoretical
ratio between NEAs with retrograde and prograde rotation $N_r/N_p$ can be estimated to be: 
(Bottke et al. 2002.):\\

$N_r/N_p \approx (1+P_{\nu_6})/(1-P_{\nu_6}) \approx 2 \pm 0.2$, \\

\noindent
where $P_{\nu_6}$ is a probability that the object comes from $\nu_6$ resonance. 
This resonace is very effective and lies at the inner edge of the main belt and therefore 
can be reached due to Yarkovsky drift only by objects evolving inward, so retograde rotators.
All other resonances can be reached by objects drifting inward and outward, that is prograde 
and retrograde spinning.\\

The present data give surprisingly good fit. The ratio between retrograde and prograde rotators 
is (Fig.2): \\

$N_r/N_p = 2$. \\

\noindent
This result confirms the key role of the Yarkovsky effect in production of NEAs (H1).\\

\begin{figure}
\begin{center}
\includegraphics[width=8cm,height=10cm,angle=-90]{aa.eps}
\end{center}
\caption{The figure represents, in a sinusoidal equal--area 
carthographic representation, the pole distributions of asteroids in ecliptic 
reference frame. The different symbols represents MBA's and NEAs of different sizes. 
The Koronis family asteroids are starred.}
\end{figure}

Detailed statistical analysis of the spin parameters of the MBAs is 
presented in the publication H2.
The distribution of the ecliptic latitudes of the spin vectors of MBAs is different 
than in case of NEAs, described above.
Especially we observe a lack of objects which spin vector lies close to the ecliptic plane
(Fig.1). There is also no excess of the prograde rotators among the largest MBAs,
often claimed as a remnant from the formation of the Solar System.
From the other hand we observe an excess of the prograde rotators among objects smaller than
100--150~m.

During this study we searched for the evidence of the influence of the YORP effect on small MBAs, 
of diameters D<60~km. Unfortunately objects smaller than 40~km from the main belt have unknown 
spin vectors, except of the members of the Koronis family.
It appeared that the spin vectors of small asteroids are clustered toward the ecliptic poles 
in comparison with the larger bodies (Fig.3). This result suggests that the positions of the 
spin axes of small MBAs were modified by YORP. 

Unfortunately the number of small MBAs sensitive to the non-gravitational effects,  
with known spin parameters, is still insufficient. In the publication H2 I highlighted the need 
to further study of those objects objects, especially members of the dynamical families. \\

\begin{figure}
\begin{center}
\includegraphics[width=9cm,height=6cm]{maxwell.eps}
\end{center}
\caption{Solid line - observed rotation-rate distribution for 142 objects of the Flora family <35~km.
Asteroids observed within the campaign (described in H4) are marked in grey.
The dashed curve represents the Maxwellian distribution, for a mean squared frequency of 5.47 1/d.}
\end{figure}

In the articels H4 and H5 I investigated the fingerprints of the Yarkovsky and YORP effects on asteroids 
from the Flora family. The Flora family lies at the inner part of the main belt 
and consists of many small asteroids, more than 10~000 (Nesvorny 2010), almost all of them 
smaller than 30~km. 

\begin{figure}[t]
\begin{center}
\includegraphics[width=12cm,height=9cm]{Lundia3.eps}
\end{center}
\caption{Observed lightcurves of the binary asteroid Lundia depending on the orientaion of the system to 
         the line of sight. Eclipses visible on 5 lightcurves from 2005/2006 opposition. Eclipses in 
         the system are not visible in the lightcurve from 2007.}
\end{figure}


The Flora family existing in the inner main belt is located close to the $\nu_6$ secular resonance with Saturn. 
Photometric observations of this family were carried out at 15 different observatories, using telescopes 
up to 2.5~m in diameter, thanks to 30 observers. The obtained lightcurves allowed me to determine, 
correct or confirm synodic periods of the observed asteroids.
The results of the observing campaign are described in the publication H4, which presents more than 540
lightcurves of 55 asteroids.
Statistical analysis of the spin rates of the Flora family asteroids (Fig.4) was supplemented with the 
91 objects of known and published spin rates. 

The rotation-rate distributions of the observed sample of 55 asteroids and the whole sample of 142 objects 
look very similar. The theoretical distribution of the spin rates of objects of the family 
which was formed in a catastrophic collision should be Maxwellian (Fig.4).
The Kolmogorov - Smirnov one sample test confirms that the distribution of rotation-rates in the Flora 
family is inconsistent with a Maxwellian distribution at a confidence level of 94\%. 
We see an excess of fast and slow rotators most probably connected with the YORP effect and a peak around 
4-5 rotations per day, which might still be connected with the original spin rate of the family parent body.
The distribution of spin rates in the Flora family presented in Fig.4 differs significantly from the 
distribution reported for the Koronis family by Slivan et al. (2008) and the Hungaria family by Warner et al. 
(2009) and suggests younger age of the Flora family. This result confirms former studies of the surface of 
951~Gaspra (member of the Flora family) based on the observations from Galileo spacecraft (Chapman 2002).\\

Photometric observations of the Flora family asteroids allowed me to discover binary nature of 809~Lundia.
The details I present in the article H3. Some lightcurves of binary asteroids show sudden 
drops in brightness of about 0.75~mag, which reperesent similar sizes of the components of the system.
Additionally between sharp minima the ,,shoulder-like shape'' connected with the attenuation events and 
rotation of nonspherical components is visible. 
Figure 5 shows the observed lightcurves of 809~Lundia depending on the orientation of the system 
to the line of sight.

Such binaries (only 13 known in the Solar System) rotate synchronously or almost synchronously 
with periods longer than 13.5~h. 809~Lundia, known for almost 100 years, appeared to be such binary.
It is very interesting object of V taxonomic type (basaltic surface similar to the asteroid 4~Vesta), 
but dynamically connected with the Flora family. Taxonomically Lundia do not fit to the other 
Flora family members which are of the same S taxonomic type (silicate).
V-type suggests the origin of Lundia from 4~Vesta. It is known that Vesta suffered a gigantic collision 
about 1 billion years ago, which was a source of the only V-type asteroid family.

Carruba et al. (2005) analysed the possible migration of Lundia due to resonances and Yarkovsky effect 
on its current orbit, but they assumed single retrograde rotating body. The obtained migration time 
was about 1.2 billion years, that suggested the relationship to the Vesta family.
The results of the photometric observations of Lundia are presented in the publication H3.
The modelling of the system done using two different methods, based on the obtained lightcurves, gave
ecliptic coordinates of the pole of the orbit of the system $\lambda=119 \pm 2^\circ$, $\beta=28 
\pm 4^\circ$ (in Roche model) or $\lambda=120 \pm 5^\circ$ $\beta=18 \pm 12^\circ$ (in kinematic model) 
which means that the system rotates prograde. 
It is hard to explain migration of such system with effects described by Carruba et al. (2005). 
Additionally other parameters of the system were obtained: distance between components 15.8~km, 
sizes of the components of about 8~km, asuming the equivalent diameter of the single body $9.1~km$ and 
absolute brightness $H=11.8$ mag, and albedo $p_V=0.4$, period of rotation $15.418 \pm 0.001 h$,
and density of the bodies about $\rho= 1.7 g/cm^3$. The obtained density in comparison with the HED 
meteorites comming from Vesta ($2.86 - 3.26g/cm^3$) means that the porosity of the Lundia components 
is of about 42-49\%. Density and porosity are the most important parameters describing 
internal structure of the small bodies and are possible to determine thanks to binary systems. \\

\begin{figure}
\begin{center}
\includegraphics[width=9cm,height=6cm]{F3a.eps}
\end{center}
\caption{Positions of prograde (blue dots) and retrograde
(red dots) asteroids in proper-element space: orbit semimajor axis {\it a}
[AU] versus eccentricity {\it e}. The grey path shows the position of $\nu_6$ resonance
(which depends on orbit inclination).}
\end{figure}

The results obtained during 10-year long observing campaign of the Flora family asteroids I used for 
searching for the fingerprints of the Yarkovsky and YORP effects in this family.
The last article H5 presents the results of modelling of 16 asteroids. For each of them about 
20 lightcurves were obtained at different observing circumstances.
Such big number of lightcurves is necessary for modelling (spin axis orientation, sidereal spin rate 
and shape) using lightcurves inversion method (Kaasalainen \& Torppa 2001, Kaasalainen et al. 2001).

It is known that the Yarkovsky effect moves small astroids to larger/smaller semimajor
axes depending on their prograde/retrograde spins. Splitting of asteroid families into prograde 
and retrograde groups has been recently proposed as a result of the Yarkovsky effect (Vokrouhlicky 1998, 
Vokrouhlikcy 1999, Vokrouhlicky \& Farinella 1998, Bottke et al. 2001, Morbidelli \& Vokrouhlicky 2003, 
Spitale \& Greenberg 2001). Prograde and retrograde asteroids drift in different directions but this 
has never been observed directly.

Results of modelling of the Flora family asteroids show the family splitting into prograde (marked as 
blue dots) and retrograde (marked as red dots) groups as a result of the Yarkovsky effect (Figs. 6 and 7). 

Moreover the retrograde objects drifting inward reach the $\nu_6$ resonace which is an escape channel 
for production of NEAs. The location of the Flora family close to the $\nu_6$ resonace explains
the lack of retrograde objects and confirms the excess of retrograde rotators 
among NEAs and their origin from the $\nu_6$ (described in article H1). \\

\begin{figure}
\begin{center}
\includegraphics[width=9cm,height=6cm]{F5.eps}
\end{center}
\caption{Absolute magnitude H (mag) as a function of semimajor
axis a (AU) for Flora family asteroids. The grey circles represent 123
Flora family objects with known spin periods of rotation (smaller than 30 km).
The positions of retrograde are shown as red dots, and prograde as blue dots.
The largest members of the family - 8~Flora and 43~Ariadne - are also presented.}
\end{figure}


Almost all objects smaller than 40~km in the main belt, of known spin parameters, belonged to the 
Koronis family. These asteroids have correlated rotation rates and aligned spin vectors (Slivan 2002, 2009) 
caused by YORP effect and spin-orbit resonaces (Vokrouhlicky et. al 2003). 
Objects trapped in the resonance were said by Vokrouhlicky et al. (2003) to be in a Slivan state.
Vokrouhlicky et al. (2003) predicts that only outer belt asteroids might be found in Slivan states. 
The comparison of the theory with the observation was in interesting challenge.

It appeared that also in the Flora family the alignment of spin vectors and correlation of spin rates
is visible, similarly as in the case of the Koronis family, caused most probably by YORP.
Figure 8 presents the comparison of the position of the spin vectors and spin rates for both families 
(squares for the Koronis family, dots for the Flora family). The similar positions for both families are 
clearly visible. The figure was done in the same convention as in Slivan (2003), the orbital latitude 
of the spin vector is presented. (In most cases in the main belt the inclination of the orbit 
to the ecliptic plane is low so the ecliptic and orbital coordinates of the spin vector are very close.)
This result is unexpected and suggests that the theory of YORP requires some improvement and that
the Slivan states might be more common than the theory predicted. \\

%\vspace{1cm}
\begin{figure}
\begin{center}
\includegraphics[width=9cm,height=6cm]{F2.eps}
\end{center}
\caption{Relation between spin vector obliquity and rotation frequency
of the Flora (blue and red dots) and the Koronis (green and brown squares) family members. 
Dots and squares of different pattern represent stray objects, that does not seem to fit to 
the grouping The abscissa are defined with the same convention as in Slivan (2002).}
\end{figure}

\subsection{Conclusions}

The publications presented above are devoted to the observational verification of the influence of the 
Yarkovsky and YORP effects on asteroids. The main achievents are listed below:

\begin{itemize}
\item Continuation and regular updates of the ,,Asteroid spin vector determinations database''.
\item Explanation of the origin of NEAs from $\nu_6$ resonance due to Yarkovsky drift.
\item Statistical analysis of the main belt asteroids spin axis distribution and founding the influence 
      of the YORP effect on the smallest objects in the database. 
\item Discovery of the binary nature of the asteroid 809~Lundia and determination of its model, which
      is inconsistent with the adopted one to the explanation of the position 
      of Lundia on its current orbit.
\item Organization of the international photometric observing campaign of the Flora family asteroids.
\item Explanation of the observed rotation-rate distribution of the Flora family asteroids by the 
      YORP effect and estimation of the age of the family.
\item Discovery of the Flora family splitting into prograde and retograde groups as a result of the 
      Yarkovsky effect.
\item Discovery of the similar latitudes and spin rates (Slivan states) among the Flora family asteroids 
      caused most probably by YORP effect.
\item Confirmation of the origin of NEAs from the Flora family due to the Yarkovsky drift to the $\nu_6$ resonance.

\end{itemize}

\subsection*{References}

Bottke, W. F. Vokrouhlicky, D., Broz, M., Nesvorny, D. \& Morbidelli,
2001, Science 294, 1693\\

\noindent
Bottke, W.F., Vokrouhlicky, D., Rubincam, D.P. \&
Broz, D.P. 2002, In Asteroids III, W.F. Bottke, A. Cellino, P. Paolicchi,
\& R.P. Binzel (Univ. Arizona Press, Tucson), 395 \\

\noindent
Chapman, C.R. 2002 in Asteroids III, W.F. Bottke, A. Cellino,.
P. Paolicchi, \& R.P. Binzel. (Univ. Arizona Press, Tucson), 315\\

\noindent
Carruba V., Mitchenko T.A., Roig F., Ferraz-Mello S.,
Nesvorny D. 2005, A\&A, 441, 819\\

\noindent
Kaasalainen, M. \& Torppa, J. 2001, Icarus 153, 24\\

\noindent
Kaasalainen, M., Torppa, J. \& Muinonen, K. 2001, Icarus 153, 37\\

\noindent
Morbidelli, A. \& Vokrouhlicky, D. 2003,
Icarus 163, 120\\

\noindent
Nesvorny, D. 2010, Nesvorny HCM Asteroid Families V1.0. \\
EAR-A-VARGBDET-5-NESVORNYFAM-V1.0. NASA Planetary Data System \\

\noindent
Slivan, S.M., 2002, Nature 419, 49 \\

\noindent
Slivan, S.M., Binzel, R.P., Boroumad, S.C., et al. 2008,
Icarus 195, 226 \\

\noindent
Slivan, S.M., Binzel, R.P., Kaasalainen M., et al. 2009,
Icarus 200, 514\\

\noindent
Spitale, J., \& R. Greenberg, 2001, Icarus 149, 222\\

\noindent
Vokrouhlicky, D., 1998, A\&A 335, 1093\\

\noindent
Vokrouhlicky, D., 1999, A\&A 344, 362\\

\noindent
Vokrouhlicky D. \& Farinella, P. 1998, AJ 116, 2032\\

\noindent
Vokrouhlicky, D., Nesvorny D., Bottke, W.F. 2003,
Nature 425, 147\\

\noindent
Warner, B., Harris, A.W., Vokrouhlicky, D.,
et al. 2009b, Icarus 204, 172\\


\section{Description of the other scientific achievements}

My whole scientific career I devoted to study physical properties of asteroids. I planned and 
observed asteroids in Borowiec, Poznań, Ostrowik, Pic du Midi (France), Rozhen (Bulgaria) and 
other observatories. I reduced data and did photometry from the observatories mentioned above 
and many others in the World. For more than 15 years I am working on archiving of all observing 
data from Borowiec photometric telescope. 

At the beginning the goal of my study were selected main belt asteroids. New photometric obervations 
carried out within few years combined with the already published lightcurves allowed for the first 
spin vector and shape determination for many objects.
New models enlarge the number of asteroids included in the ,,Asteroid spin vector determinations 
database'' and were the basis of statisticals analysis.
Among the studied bodies were asteroids of the longest spin period like 288~Glauke, or tumblers like 
4179~Toutatis.

A part of my work was devoted to asteroid binary systems, among them 90~Antiope, the largest synchronous 
binary in the Solar System, each body of 85~km of diameter.
Another studied binary asteroid 22~Kalliope has 166~km in diameter. Its satellite Linus 
is very small and has only 28~km of diameter. Both types of binary systems are the sources of fundamantal 
parameters describing small Solar System bodies --- density and macroporosity.

My other research were connected with observations and modelling of asteroids 21~Lutetia and 2867~Steins 
--- both targets of the space mission Rosetta. 
Thanks to this work we confirmed the correctness of the ground-based methods of asteroids modelling,
especially lightcurve inversion method.

A part of my research was devoted to the photometric observations of very small NEAs. We used South African 
Large Telescope (SALT). I took part in planning and reduction of the photometric data from SALT.
Among the others we observed $2006 RH_{120}$, the temporary Earth satellite.

In addition to the Flora family I studied the asteroids members of the Datura family, 
which age is estimated to only 530 million years.
Recently my research was focussed also on the asteroids spectroscopy. The inspiration of such studies 
was asteroid 809~Lundia. Just after the discovery of the binary nature of Lundia I would like to check
if both components of the system are of the same taxonomic type. Thanks to the cooperatrion with Paris 
Observatory, we were able to observe Lundia using a 3~m IRTF (Infrared Telescope Facility) located in 
Mauna Kea, Hawaii. Our observations confirmed similar properties of the surface of both components 
of the Lundia system. The results were presented during several international conferences. 
The publication based on the spectroscopic data, obtained during few observing runs at different 
observing circumstances, as well as modelling of the surface,  was already submitted to the 
Monthly Notices (Spectroscopy and surface properties of binary asteroid 809~Lundia, 
Birlan M. et al.).

\subsection{Authorship and co-authorship of scientific publications}
I am a coauthor of 35 publications from  Journal Citation Reports (JCR) database, part A, 
32 of them were published before my Ph.D. thesis.
I am also author and/or coauthor of 28 other publications.
The total Impact Factor of my publications is 147,957.
The total citation index based on the Web of Knowledge is 372 (280 without autocitations), 
based on the SAO/NASA Astrophysic Data System (ADS) 392.
My Hirsch index is 12. \\
\noindent
Detailed list of publications is attached to this document.\\

\subsection{Leadership and participaion in the scientific projects}

\noindent
Polish Committee of Scientific Research Junior Grant (2.P03D.022.09) \\
Project manager A. Kryszczyńska, 01.07.1995 -- 30.06.1996\\

\noindent
Polish Committee of Scientific Research Grant (2.P03D.024.09), participant,
01.07.1995 -- 31.12.1998, manager of the project prof. T. Michałowski\\

\noindent
Polish Committee of Scientific Research Grant (2.P03D.007.018), participant,
01.01.2000 -- 30.09.2003, project manager prof. T. Michałowski\\

\noindent
Polish Committee of Scientific Research Grant (2.P03D.007.022), participant,
01.04.2002 -- 31.03.2005, project manager Dr. hab. T. J. Jopek\\

\noindent
Tempus-Structural and Complementary Measures, Grant No. C016A05-2005, 
Investigations of Market Needs of Various Physics 
Study Profiles: A New Supplement Diploma for Physics Studies, 
Consortium among Universities of Skopje (MK), Ferrara (I), Poznan (PL), Tetovo (MK), 
Ministry of Education and Sciences (MK).
Partner country representative -- A. Kryszczyńska, 11.2005 -- 11.2006 \\

\noindent
Polish Committee of Scientific Research Grant (1 P03D 008 026), 
project manager Dr. A. Kryszczyńska, 26.04.2004 -- 26.12.2007\\ 

\noindent
Polish Ministry of Science and High Education Grant/National Center for 
Science Grant (N N203 382136), project manager Dr. A. Kryszczyńska,\\ 
27.03.2009 -- 26.05.2012\\

\subsection{Awards and honors}

\begin{itemize}\setlength{\itemsep}{-0.5\baselineskip}
\item Individual Award of the Rector of A. Mickiewicz University, for 
scientific achievements, 2005. 

\item Two Team Awards of the Rector of A. Mickiewicz University, for 
scientific achievements, 2008.

\item In July 2008 the Committee on Small Body Nomenclature (International 
Astronomical Union) gave a name Kryszczynska to the asteroid 21776 (1999 RE221), 
for my contribution to the study of asteroids, especially for the discovery of 
the binary nature of the asteroid 809~Lundia and for maintaining a database
of asteroid spin vector determinations. \\

{\it The following citation of IAU CSBN is from MPC 63394:
(21776) Kryszczyńska = 1999 RE221 Agnieszka Kryszczyńska (b. 1965) is a
planetary scientist at Adam Mickiewicz University, Poznań. Using photometry,
she has studied the physical properties of minor planets. She discovered the
binary nature of (809) Lundia and maintains a database of the pole
coordinates and shapes of minor planets.}\\

\item Team Award of the Rector of A. Mickiewicz University, for
      scientific achievements, 2010.

\item Dean of the Physics Department Award, for preparing new programs of studies 
      of astronomy, 2013.

\item Highlighting the publication H5 by {\it Astronomy and Astrophysics} editors, 2013.
\end{itemize}


\subsection{Participation and organization of international conferences}

\begin{enumerate}

\item Dynamics and astrometry of natural and artificial celestial bodies, 
Poznań, Poland, 1993
\item
IAU Coll. 165, Dynamics and astrometry of natural and artificial celestial 
bodies, Poznań, Poland, 1996 -- secretary of LOC, 2 posters
\item
Asteroids Comets Meteors 1996, Versailles, France, 1996,
3 posters
\item
IAU Coll. 173, Evolution and source regions of asteroids and comets,
Tatranska Lomnica, Slovak Republic, 08.1998,
poster
\item 
Asteroids Comets Meteors 1999, Ithaca, USA,1999, 
3 posters
\item
Asteroids 2001, Palermo, Italy, 2001, 
2 poster
\item
Ceres 2001 Workshop, Paris, France, 10.2001, 2 posters
\item
Asteroids Comets Meteors 2002, Berlin, Germany, 2002,
5 posters
\item 
Italian Planetary Sciences Meeting, Gallipoli, Italy, 2003, 
coauthor of the lecture without participation in the conference
\item
Balkan Astronomical Meeting, NAO Rozhen, Bulgaria, 2004,
invited lecture
\item
Asteroids Comets Meteors 2005, Buzios, Rio de Janeiro, Brazil, 2005, 
3 posters
\item
6th General Conference of the Society of Physicists 
of the Republic of Macedonia, Ohrid, Macedonia, 2006,
lecture
\item
Division for Planetary Sciences of the American Astronomical Society
Meeting (DPS) 2006, Pasadena CA, USA, poster without participation in the conference
\item 
Workshop on Astrophysics and Space Research, Serock 
near Warsaw Poland, 06.2007, oral presentation
\item
First Worshop on Binaries in the Solar System, Steamboat 
Springs, Colorado, USA, 2007,
oral presentation
\item 
Asteroids Comets Meteors 2008, Baltimore USA, 2008,
3 posters
\item 
Workshop on Binaries in the Solar System II, Poznań,
Poland, 2010 -- main organizer, \\
{\em http://www.boulder.swri.edu/binaries2-mtg/},
oral presentation
\item 
Division for Planetary Sciences of the American Astronomical Society
Meeting (DPS) 2010, Pasadena CA, USA, poster without participation in the conference
\item 
Asteroids Comets Meteors 2012, Niigata, Japonia,
oral presentation and 2 posters
\item
XIXth Meeting of the Petrology Group of the Mineralogical 
Society of Poland ,,Meteorites: Insights into Planetary Compositions'', 2012,
invited lecture
\item
Asteroid Spectroscopy in Support of Gaia (ASSG2013), Nice, France, 2013,
\item 
3rd Workshop on Binaries in the Solar System, Kohala Coast, Big Island, 
Hawaii, USA, 2013,\\
oral presentation

\end{enumerate}

\subsection{Local conferences}
\begin{enumerate} 
\item
Meetings of the Polish Astronomical Society 1991, 1995, 
1999, 2001, 2003, 2005, 2007, 2009, 2011
\item
Meetings of Polish Meteoritical Society 2005, 2007
\item
Astronomy at small telescopes Kielce 2005, Kraków/Koninki 2013 
\item
Celestial Mechanics Seminars 2004, 2005, 2006
\item Astronomy of XXI century and its teaching, Niepołomice, 2008, 
2009

\end{enumerate}
During all meetings lecture or poster was presented.


\subsection{Membership in international and local organizations and
scientific societies}

\begin{itemize}
\item Member of the Polish Astronomical Society, from 2005 member of management 
of the Society

\item Member of the International Astronomical Union

\end{itemize}

\subsection{Visits at foreign scientific institutes or universities}

\begin{itemize}
\item France, Bureau des Longitudes, two one-month scholarships of the French Government
          (CNRS) 1994, 1995
\item France, many observing runs at Pic du Midi Observatory
\item France, visiting astronomer, Paris Observatory, 1 month, 1997
\item Bulgaria, several observing runs at NAO Rozhen
\item France, many visits at the Institute de Mecanique Celeste et de Calcul 
          des Ephemerides, Observatoire de Paris
\item USA, Southwest Research Institute, Boulder, Colorado, (invitation from Dr. William Merline).
          During this visit observations of asteroids using AO at the Keck II telescope, Hawaii.
\end{itemize}

\subsection{Reviews} 
\noindent
Review of the Ph.D thesis of Gordana Apostolovska from Faculty of Natural Sciences 
and Mathematics, Sts. Ciril and Methodius University, Skopje, Republic of Macedonia 
 ,,Determination of some dynamical characteristics of chosen asteroids'', 2004.\\
\noindent
Reviews of the publications submitted to Icarus, Meteoritics and Planetary Science, 
Planetary and Space Science, Astronomy and Astrophysics.

\end{document}


